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DTSTART:20231029T030000
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TZOFFSETTO:+0100
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BEGIN:DAYLIGHT
DTSTART:20240331T020000
TZOFFSETFROM:+0100
TZOFFSETTO:+0200
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BEGIN:VEVENT
UID:ai1ec-23304@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Esami
CONTACT:
DESCRIPTION:
DTSTART;VALUE=DATE:20220307
DTEND;VALUE=DATE:20220308
LOCATION:Aula
SEQUENCE:0
SUMMARY:esami corso di management
URL:http://www.astropa.inaf.it/evento/esami-corso-di-management/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n
\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23416@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:
DTSTART;VALUE=DATE:20220404
DTEND;VALUE=DATE:20220405
SEQUENCE:0
SUMMARY:Prova Oculus e Visita studenti di Fisica G. Peres
URL:http://www.astropa.inaf.it/evento/prova-oculus-e-visita-studenti-di-fis
ica-g-peres/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23654@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Salvatore Speziale\; salvatore.speziale@inaf.it
DESCRIPTION:Riprese fotografiche di due strumenti del museo.\nRiprese fotog
rafiche dei quadri presenti al museo.\nPer documentazione interna.
DTSTART;VALUE=DATE:20220629
DTEND;VALUE=DATE:20220701
LOCATION:Museo
SEQUENCE:0
SUMMARY:Riprese fotografiche al museo
URL:http://www.astropa.inaf.it/evento/riprese-fotografiche-al-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRiprese fotografiche di due strumenti del museo.
\nRiprese fotografiche dei quadri presenti al museo.
\nPer docum
entazione interna.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23668@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Salvatore Speziale\; salvatore.speziale@inaf.it
DESCRIPTION:Foto per documentazione interna.
DTSTART;VALUE=DATE:20220801
DTEND;VALUE=DATE:20220806
SEQUENCE:0
SUMMARY:Riprese fotografiche dei quadri del museo (completamento)
URL:http://www.astropa.inaf.it/evento/riprese-fotografiche-dei-quadri-del-m
useo-completamento/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nFoto per documentazione interna.
\n
X-TAGS;LANGUAGE=it-IT:Foto\,museo
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23930@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Salvatore Speziale\; 233457\; salvatore.speziale@inaf.it
DESCRIPTION:
DTSTART;VALUE=DATE:20220927
DTEND;VALUE=DATE:20221001
SEQUENCE:0
SUMMARY:Rilievo fotografico\, di due strumenti\, per modelli 3d
URL:http://www.astropa.inaf.it/evento/rilievo-fotografico-di-due-strumenti-
per-modelli-3d/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24154@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Antonio Maggio
DESCRIPTION:
DTSTART;VALUE=DATE:20221125
DTEND;VALUE=DATE:20221126
SEQUENCE:0
SUMMARY:Meeting THE StellaR PAth
URL:http://www.astropa.inaf.it/evento/meeting-the-stellar-path/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
X-TAGS;LANGUAGE=it-IT:RIUNIONE
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24513@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Liggio
DESCRIPTION:
DTSTART;VALUE=DATE:20221214
DTEND;VALUE=DATE:20221220
LOCATION:scala accesso museo
SEQUENCE:0
SUMMARY:intervento di manutenzione e messa a norma scala di accesso al muse
o (a cura di UNIPA)
URL:http://www.astropa.inaf.it/evento/intervento-di-manutenzione-e-messa-a-
norma-scala-di-accesso-al-museo-a-cura-di-unipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26295@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Concorso\,Aula: Esami
CONTACT:FILIPPO SALEMI
DESCRIPTION:
DTSTART;VALUE=DATE:20231113
DTEND;VALUE=DATE:20231118
LOCATION:AULA PIAZZI
SEQUENCE:0
SUMMARY:ESAMI
URL:http://www.astropa.inaf.it/evento/esami/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26974@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Salvatore Speziale\; salvatore.speziale@inaf.it
DESCRIPTION:Progetto di modellazione fotogrammetrica per la creazione di mo
delli 3d degli interni del museo e delle collezioni.\n
DTSTART;VALUE=DATE:20240121
DTEND;VALUE=DATE:20240125
SEQUENCE:0
SUMMARY:Riprese fotografiche per modellazione vetrina e consolle di Dufourn
y
URL:http://www.astropa.inaf.it/evento/riprese-fotografiche-per-modellazione
-vetrina-e-consolle-di-dufourny/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nProgetto di modellazione fotogrammetrica per la cre
azione di modelli 3d degli interni del museo e delle collezioni.
\n
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-21681@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:stanza Google meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Ileana Chinnici (INAF)\nTitolo: Forse non tutti sanno che … : piccoli
e grandi appuntamenti dell’Osservatorio di Palermo con la storia\nAbstract
: Con questo seminario si intende illustrare brevemente il ruolo avuto dal
l’Osservatorio di Palermo nella storia dell’astronomia\, ripercorrendo sco
perte ed eventi di varia rilevanza\, avvenuti nel suo primo secolo di stor
ia. Si è trattato di un periodo particolamente vivace ed interessante\, in
cui non sempre si è avuta consapevolezza dell’importanza storica di quant
o stava avvenendo in Osservatorio. Proveremo a rileggere la storia di ques
ta istituzione con uno sguardo più attento ai particolari.
DTSTART;TZID=Europe/Rome:20210415T150000
DTEND;TZID=Europe/Rome:20210415T163000
SEQUENCE:0
SUMMARY:Seminario: I. Chinnici (INAF)\, 15 Aprile 2021 ore 15.00
URL:http://www.astropa.inaf.it/evento/seminario-i-chinnici-inaf-4-marzo-202
1-ore-15-00/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nstanza Google meet: https://meet.google.com/sxz-cct
p-tsc
\nSpeaker: Ileana Chinnici (INAF)
\nTitolo: Forse non tu
tti sanno che … : piccoli e grandi appuntamenti dell’Osservatorio di Paler
mo con la storia
\nAbstract: Con questo seminario si intende illustr
are brevemente il ruolo avuto dall’Osservatorio di Palermo nella storia de
ll’astronomia\, ripercorrendo scoperte ed eventi di varia rilevanza\, avve
nuti nel suo primo secolo di storia. Si è trattato di un periodo particola
mente vivace ed interessante\, in cui non sempre si è avuta consapevolezza
dell’importanza storica di quanto stava avvenendo in Osservatorio. Prover
emo a rileggere la storia di questa istituzione con uno sguardo più attent
o ai particolari.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22100@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Vincenzo Sapienza (UNIPA)\nstanza Google Meet: meet.g
oogle.com/sxz-cctp-tsc\nTitolo: X-ray emitting structures in the Vela SNR:
Ejecta anisotropies and progenitor stellar wind residuals.\nAbstract: L’e
splosione di una stella massiva come supernova crea uno shock supersonico\
, detto forward shock\, si propaga attraverso il mezzo interstellare (ISM)
e un reverse shock colpisce e spazza il materiale appartenente alla stell
a progenitrice\, che viene espulso a migliaia di km/s e prende il nome di
ejecta.\nL’interazione del forward shock con l’ISM e del reverse shock con
gli ejecta riscalda il plasma fino a temperature alle quali il plasma eme
tte nei raggi X.\nLo studio dell’emissione nei raggi X proveniente dai res
ti di supernova (SNR) fornisce un potente strumento per studiarli e da que
sto\, indirettamente\, dedurre i meccanismi che governano l’esplosione di
una supernova\, dal momento che questi non posso essere esplorati con osse
rvazioni dirette\, e vincolare il comportamento di stelle massive negli st
adi finali della loro vita.\nIl resto di supernova galattico delle Vele è
una sorgente ideale per questo tipo di studi\, essendo il resto di superno
va più vicino a noi.\nEsso mostra diversi frammenti di ejecta (o shrapnel)
che protrudono dallo shock esterno.\nRecenti studi hanno rivelato una abb
ondanza di silicio (Si) in due shrapnel (lo shrapnel A e lo shrapnel G)\,
osservati in due punti del SNR quasi esattamente opposti rispetto al centr
o del SNR.\nQuesto suggerisce la presenza di una struttura a getto e contr
o-getto ricca di silicio\, simile a quanto osservato nel SNR di Cassiopea
A.\nPer mettere alla prova questo scenario abbiamo analizzato una osservaz
ione XMM-Newton di una regione luminosa nei raggi X\, denominata “knot K”
e localizzata subito dietro lo shrapnel G e lungo la congiungente degli sh
rapnel A e G\, con il fine di studiarne le proprietà fisiche e chimiche pe
r accertare la presenza di una struttura facente parte di questa possibile
struttura a getto e contro-getto.\nAbbiamo prodotto mappe del count-rate
sottratte di background (e smussate adattivamente) e mappe di energia medi
ana dei fotoni e abbiamo effettuato un’analisi spettrale spazialmente riso
lta.\nAbbiamo individuato la presenza di due strutture con diverse proprie
tà fisiche e chimiche all’interno del campo di vista.\nLa prima è marcatam
ente elongata in direzione delle congiungente degli shrapnel A e G (e del
centro del SNR).\nIl suo spettro nei raggi X è molto più soffice di quello
degli shrapnel ricchi di Silicio e questo ostacola la determinazione dell
a abbondanza di questo elemento\, comunque le proprietà fisiche e chimiche
sono consistenti con con gli shrapnel A e G.\nLa seconda struttura\, che
nell’osservazione si estende nella direzione nord-ovest sud-est\, mostra u
na temperatura significativamente più alta e appare come un filamento sott
ile.\nAnalizzando dati di archivio ROSAT del resto abbiamo trovato che que
sto filamento appartiene ad una struttura su grandissima scala (∼20 pc) e
coerente\, che abbiamo identificato vicino al bordo ovest del SNR.\nAbbiam
o dunque ottenuto una descrizione approfondita della coda elongata dello s
hrapnel G lasciata dietro dal suo moto supersonico.\nInoltre abbiamo scope
rto una struttura molto estesa che abbiamo interpretato come segno del’int
erazione tra il resto di supernova e il vento stellare della stella progen
itrice.\nIl peculiare rapporto Ne/O che abbiamo trovato potrebbe suggerire
una progenitrice Wolf-Rayet per il resto di supernova delle Vele\, tuttav
ia per affrontare questo aspetto serviranno ulteriori analisi.
DTSTART;TZID=Europe/Rome:20210420T150000
DTEND;TZID=Europe/Rome:20210420T160000
SEQUENCE:0
SUMMARY:Seminario: Vincenzo Sapienza (UNIPA) 20 Aprile ore 15
URL:http://www.astropa.inaf.it/evento/seminario-vincenzo-sapienza-unipa-20-
aprile-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Vincenzo Sapienza (UNIPA)
\nstanza G
oogle Meet: meet.google.com/sxz-cctp-tsc
\nTitolo: X-ray emitting s
tructures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind
residuals.
\nAbstract: L’esplosione di una stella massiva come supe
rnova crea uno shock supersonico\, detto forward shock\, si propaga attrav
erso il mezzo interstellare (ISM) e un reverse shock colpisce e spazza il
materiale appartenente alla stella progenitrice\, che viene espulso a migl
iaia di km/s e prende il nome di ejecta.
\nL’interazione del forward
shock con l’ISM e del reverse shock con gli ejecta riscalda il plasma fino
a temperature alle quali il plasma emette nei raggi X.
\nLo studio d
ell’emissione nei raggi X proveniente dai resti di supernova (SNR) fornisc
e un potente strumento per studiarli e da questo\, indirettamente\, dedurr
e i meccanismi che governano l’esplosione di una supernova\, dal momento c
he questi non posso essere esplorati con osservazioni dirette\, e vincolar
e il comportamento di stelle massive negli stadi finali della loro vita.\nIl resto di supernova galattico delle Vele è una sorgente ideale per
questo tipo di studi\, essendo il resto di supernova più vicino a noi.
\nEsso mostra diversi frammenti di ejecta (o shrapnel) che protrudono d
allo shock esterno.
\nRecenti studi hanno rivelato una abbondanza di
silicio (Si) in due shrapnel (lo shrapnel A e lo shrapnel G)\, osservati i
n due punti del SNR quasi esattamente opposti rispetto al centro del SNR.<
br />\nQuesto suggerisce la presenza di una struttura a getto e contro-get
to ricca di silicio\, simile a quanto osservato nel SNR di Cassiopea A.
\nPer mettere alla prova questo scenario abbiamo analizzato una osserva
zione XMM-Newton di una regione luminosa nei raggi X\, denominata “knot K”
e localizzata subito dietro lo shrapnel G e lungo la congiungente degli s
hrapnel A e G\, con il fine di studiarne le proprietà fisiche e chimiche p
er accertare la presenza di una struttura facente parte di questa possibil
e struttura a getto e contro-getto.
\nAbbiamo prodotto mappe del coun
t-rate sottratte di background (e smussate adattivamente) e mappe di energ
ia mediana dei fotoni e abbiamo effettuato un’analisi spettrale spazialmen
te risolta.
\nAbbiamo individuato la presenza di due strutture con di
verse proprietà fisiche e chimiche all’interno del campo di vista.
\n
La prima è marcatamente elongata in direzione delle congiungente degli shr
apnel A e G (e del centro del SNR).
\nIl suo spettro nei raggi X è mo
lto più soffice di quello degli shrapnel ricchi di Silicio e questo ostaco
la la determinazione della abbondanza di questo elemento\, comunque le pro
prietà fisiche e chimiche sono consistenti con con gli shrapnel A e G.
\nLa seconda struttura\, che nell’osservazione si estende nella direzion
e nord-ovest sud-est\, mostra una temperatura significativamente più alta
e appare come un filamento sottile.
\nAnalizzando dati di archivio RO
SAT del resto abbiamo trovato che questo filamento appartiene ad una strut
tura su grandissima scala (∼20 pc) e coerente\, che abbiamo identificato v
icino al bordo ovest del SNR.
\nAbbiamo dunque ottenuto una descrizio
ne approfondita della coda elongata dello shrapnel G lasciata dietro dal s
uo moto supersonico.
\nInoltre abbiamo scoperto una struttura molto e
stesa che abbiamo interpretato come segno del’interazione tra il resto di
supernova e il vento stellare della stella progenitrice.
\nIl peculia
re rapporto Ne/O che abbiamo trovato potrebbe suggerire una progenitrice W
olf-Rayet per il resto di supernova delle Vele\, tuttavia per affrontare q
uesto aspetto serviranno ulteriori analisi.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22179@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:stanza Google Meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Darius Modirrousta-Galian (UNIPA)\nTitle: RAPOC: the Rosseland and Pla
nck opacity converter\nA user-friendly and fast opacity program for Python
\nAbstract:\nWe present a novel code that converts the widely-used wavelen
gth-dependent opacities of gaseous species into Rosseland and Planck mean
opacities. RAPOC (Rosseland and Planck Opacity Converter) is a straightfor
ward and efficient code that makes use of ExoMol data as well as any other
user-defined data\, provided that it is within the correct format. Furthe
rmore\, RAPOC has the useful ability of rapidly interpolating between disc
rete data points\, therefore allowing for a complete incorporation within
atmospheric models. In this paper we present the RAPOC code and compare it
s calculated Rosseland and Planck mean opacities with other values within
the literature.
DTSTART;TZID=Europe/Rome:20210506T110000
DTEND;TZID=Europe/Rome:20210506T123000
SEQUENCE:0
SUMMARY:Seminario: Darius Modirrousta-Galian (UNIPA)\, 6 Maggio ore 11
URL:http://www.astropa.inaf.it/evento/seminario-darius-modirrousta-galian-u
nipa-6-maggio-ore-11/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nstanza Google Meet: https://meet.google.com/sxz-cct
p-tsc
\nSpeaker: Darius Modirrousta-Galian (UNIPA)
\nTitle: RAP
OC: the Rosseland and Planck opacity converter
\nA user-friendly and
fast opacity program for Python
\nAbstract:
\nWe present a nove
l code that converts the widely-used wavelength-dependent opacities of gas
eous species into Rosseland and Planck mean opacities. RAPOC (Rosseland an
d Planck Opacity Converter) is a straightforward and efficient code that m
akes use of ExoMol data as well as any other user-defined data\, provided
that it is within the correct format. Furthermore\, RAPOC has the useful a
bility of rapidly interpolating between discrete data points\, therefore a
llowing for a complete incorporation within atmospheric models. In this pa
per we present the RAPOC code and compare its calculated Rosseland and Pla
nck mean opacities with other values within the literature.
\n
HTML>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22180@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:stanza Google Meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Sabina Ustamujiic (UNIPA)\nTitolo: Modeling the mixed-morphology super
nova remnant IC 443\nAbstract: IC 443 is a mixed-morphology (MM) SNR locat
ed in a quite complex environment\, interacting with atomic and molecular
clouds. We investigated the origin of the morphology and multi-thermal X-r
ay emission observed in SNR IC 443 through the study of the effect of the
inhomogeneous ambient medium in shaping its observed structure. We develop
ed a 3D hydrodynamic model\, which describes the interaction of the SNR wi
th the environment\, parametrized in agreement with the results of the mul
ti-wavelength data analysis. We performed an ample exploration of the para
meter space describing the model and\, from the simulations\, we synthesiz
ed the X-ray emission maps and spectra and compared them with actual X-ray
data collected by XMM-Newton. Our model explains the origin of the comple
x X-ray morphology of SNR IC 443 in a natural way\, with the ability to re
produce\, for the first time\, most of the observed features\, including t
he centrally-peaked X-ray morphology (characteristic of MM SNRs) when cons
idering the origin of the explosion at the position where the pulsar wind
nebula CXOU J061705.3+222127 was at the time of the explosion. The observe
d inhomogeneous ambient medium is the main property responsible for the co
mplex structure and the X-ray morphology\, resulting in a very asymmetric
distribution of the ejecta due to the off-centered location of the explosi
on inside the cavity formed by the clouds.
DTSTART;TZID=Europe/Rome:20210511T150000
DTEND;TZID=Europe/Rome:20210511T163000
SEQUENCE:0
SUMMARY:Seminario: Sabina Ustamujiic (UNIPA)\, 11 Maggio ore 15
URL:http://www.astropa.inaf.it/evento/seminario-sabina-ustamujiic-unipa-11-
maggio-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nstanza Google Meet: https://meet.google.com/sxz-cct
p-tsc
\nSpeaker: Sabina Ustamujiic (UNIPA)
\nTitolo: Modeling
the mixed-morphology supernova remnant IC 443
\nAbstract: IC 443 is
a mixed-morphology (MM) SNR located in a quite complex environment\, inter
acting with atomic and molecular clouds. We investigated the origin of the
morphology and multi-thermal X-ray emission observed in SNR IC 443 throug
h the study of the effect of the inhomogeneous ambient medium in shaping i
ts observed structure. We developed a 3D hydrodynamic model\, which descri
bes the interaction of the SNR with the environment\, parametrized in agre
ement with the results of the multi-wavelength data analysis. We performed
an ample exploration of the parameter space describing the model and\, fr
om the simulations\, we synthesized the X-ray emission maps and spectra an
d compared them with actual X-ray data collected by XMM-Newton. Our model
explains the origin of the complex X-ray morphology of SNR IC 443 in a nat
ural way\, with the ability to reproduce\, for the first time\, most of th
e observed features\, including the centrally-peaked X-ray morphology (cha
racteristic of MM SNRs) when considering the origin of the explosion at th
e position where the pulsar wind nebula CXOU J061705.3+222127 was at the t
ime of the explosion. The observed inhomogeneous ambient medium is the mai
n property responsible for the complex structure and the X-ray morphology\
, resulting in a very asymmetric distribution of the ejecta due to the off
-centered location of the explosion inside the cavity formed by the clouds
.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22730@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:3 persone
DTSTART;TZID=Europe/Rome:20210917T100000
DTEND;TZID=Europe/Rome:20210917T123000
SEQUENCE:0
SUMMARY:Visita Museo Emilio Molinari
URL:http://www.astropa.inaf.it/evento/visita-museo-emilio-molinari/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n3 persone
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22547@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Stanza Google Meet: meet.google.com/sxz-cctp-tsc\nSpeaker: Gabr
iele Cozzo (UniPA)\nTitolo: “Study of the accretion phenomena of T Tauri s
tars with the GRAVITY instrument”\nAbstract\nAccretion through circumstell
ar disks plays a fundamental role in the process of star formation. Charac
terising how accretion works in the context of young stellar objects will
also help us to constrain the properties of the regions in which planets f
orm and migrate. The accretion mechanism in low-mass pre-main-sequence sta
rs (T Tauri Stars) is driven by the stellar magnetic field\, which disrupt
s the disk at the magnetospheric radius\, generally located at scales of o
rder a few stellar radii. Almost bipolar field lines channel the material
from the disk to the star\, which ends with shocking at the stellar surfac
e at near free-fall velocities. From decades\, the technological improveme
nt has driven the development of new ways to probe faint and distant objec
ts as Classical T Tauri stars are and disentangle the multifarious physica
l processes involved in sustaining the stars’ evolution. The state-of-the-
art in interferometry science has indeed attained unprecedented capabiliti
es in terms of angular resolutions. This new potentiality\, coupled with t
he purpose to understand the innermost regions of CTTSs\, deserves a new a
pproach to interpret data and manipulate information. This work addresses
the ambition to lay the foundation of a new framework of observational dat
a interpretation that sheds light on the capabilities of new-class interfe
rometric instruments\, like the Very Large Telescope Interferometer\, in s
ampling and disentangling the physical conditions in which a star is born.
DTSTART;TZID=Europe/Rome:20210917T150000
DTEND;TZID=Europe/Rome:20210917T160000
SEQUENCE:0
SUMMARY:Seminario online: Gabriele Cozzo (UniPA)\, 17 Settembre\, ore 15
URL:http://www.astropa.inaf.it/evento/seminario-gabriele-cozzo-unipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nStanza Google Meet: meet.google.com/sxz-cctp-tsc
\nSpeaker: Gabriele Cozzo (UniPA)
\nTitolo: “Study of the accret
ion phenomena of T Tauri stars with the GRAVITY instrument”
\nAbstra
ct
\nAccretion through circumstellar disks plays a fundamental role i
n the process of star formation. Characterising how accretion works in the
context of young stellar objects will also help us to constrain the prope
rties of the regions in which planets form and migrate. The accretion mech
anism in low-mass pre-main-sequence stars (T Tauri Stars) is driven by the
stellar magnetic field\, which disrupts the disk at the magnetospheric ra
dius\, generally located at scales of order a few stellar radii. Almost bi
polar field lines channel the material from the disk to the star\, which e
nds with shocking at the stellar surface at near free-fall velocities. Fro
m decades\, the technological improvement has driven the development of ne
w ways to probe faint and distant objects as Classical T Tauri stars are a
nd disentangle the multifarious physical processes involved in sustaining
the stars’ evolution. The state-of-the-art in interferometry science has i
ndeed attained unprecedented capabilities in terms of angular resolutions.
This new potentiality\, coupled with the purpose to understand the innerm
ost regions of CTTSs\, deserves a new approach to interpret data and manip
ulate information. This work addresses the ambition to lay the foundation
of a new framework of observational data interpretation that sheds light o
n the capabilities of new-class interferometric instruments\, like the Ver
y Large Telescope Interferometer\, in sampling and disentangling the physi
cal conditions in which a star is born.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22566@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Stanza Google meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Ruggero Biondo (UniPA)\nTitolo: Tracing the ICME plasma with a MHD sim
ulation\nAbstract:\nThe determination of the chemical composition of Inter
planetary Coronal Mass Ejection (ICME) plasma is an open issue. More speci
fically\, it is not yet fully understood how remote sensing observations o
f the solar corona plasma during solar disturbances evolve in plasma prope
rties measured in-situ away from the Sun. The ambient conditions of the ba
ckground interplanetary plasma are important for space weather because the
y influence the evolutions\, arrival times and geo-effectiveness of the di
sturbances. The Reverse In-situ and MHD APproach (RIMAP) is a technique to
reconstruct the heliosphere on the ecliptic plane (including the magnetic
Parker spiral) directly from in situ measurements acquired at 1 AU. It co
mbines analytical and numerical approaches\, preserving the small-scale lo
ngitudinal variability of the wind flow-lines. In this work\, we use RIMAP
to test the interaction of an ICME with the interplanetary medium. We mod
el the propagation of a homogeneous non-magnetized (i.e.\, with no interna
l flux rope) cloud starting at 800 km/s at 0.1 AU out to 1.1 AU. Our 3D MH
D simulation made with the PLUTO MHD code shows the formation of a compres
sion front ahead of the ICME\, continuously driven by the cloud expansion.
Using a passive tracer\, we find that the initial ICME material does not
fragment behind the front during its propagation\, and we quantify the mix
ing of the propagating plasma cloud with the ambient solar wind plasma\, w
hich can be detected at 1 AU.
DTSTART;TZID=Europe/Rome:20210929T150000
DTEND;TZID=Europe/Rome:20210929T163000
SEQUENCE:0
SUMMARY:Seminario online: Ruggero Biondo (UniPA)\, 29 Settembre ore 15
URL:http://www.astropa.inaf.it/evento/seminario-online-ruggero-biondo-unipa
-29-settembre-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nStanza Google meet: https://meet.google.com/sxz-cct
p-tsc
\nSpeaker: Ruggero Biondo (UniPA)
\nTitolo: Tracing the
ICME plasma with a MHD simulation
\nAbstract:
\nThe determinatio
n of the chemical composition of Interplanetary Coronal Mass Ejection (ICM
E) plasma is an open issue. More specifically\, it is not yet fully unders
tood how remote sensing observations of the solar corona plasma during sol
ar disturbances evolve in plasma properties measured in-situ away from the
Sun. The ambient conditions of the background interplanetary plasma are i
mportant for space weather because they influence the evolutions\, arrival
times and geo-effectiveness of the disturbances. The Reverse In-situ and
MHD APproach (RIMAP) is a technique to reconstruct the heliosphere on the
ecliptic plane (including the magnetic Parker spiral) directly from in sit
u measurements acquired at 1 AU. It combines analytical and numerical appr
oaches\, preserving the small-scale longitudinal variability of the wind f
low-lines. In this work\, we use RIMAP to test the interaction of an ICME
with the interplanetary medium. We model the propagation of a homogeneous
non-magnetized (i.e.\, with no internal flux rope) cloud starting at 800 k
m/s at 0.1 AU out to 1.1 AU. Our 3D MHD simulation made with the PLUTO MHD
code shows the formation of a compression front ahead of the ICME\, conti
nuously driven by the cloud expansion. Using a passive tracer\, we find th
at the initial ICME material does not fragment behind the front during its
propagation\, and we quantify the mixing of the propagating plasma cloud
with the ambient solar wind plasma\, which can be detected at 1 AU.
\n<
/BODY>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22731@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:5 persone
DTSTART;TZID=Europe/Rome:20211004T113000
DTEND;TZID=Europe/Rome:20211004T130000
SEQUENCE:0
SUMMARY:visita al museo
URL:http://www.astropa.inaf.it/evento/visita-al-museo-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n5 persone
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-22726@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20211015T150000
DTEND;TZID=Europe/Rome:20211015T173000
SEQUENCE:0
SUMMARY:Visita al Museo – 20 docenti e ricercatori ERASMUS+
URL:http://www.astropa.inaf.it/evento/visita-al-museo-20-docenti-e-ricercat
ori-erasmus/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23159@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Valerio Fardella (UNIPA)\nTitolo: L’analisi delle atmo
sfere degli esopianeti. Come e perché.\nrelazione di Laurea triennale\,\ni
ndirizzo Google Meet: meet.google.com/sxz-cctp-tsc\nAbstract:\nLa composiz
ione chimica dell’atmosfera di un esopianeta può aiutare a capire quale si
ano la composizione e\, a volte\, l’evoluzione passata dell’esopianeta. L’
atmosfera\, se è presente\, può essere osservata quando il pianeta transit
a davanti la sua stella. Lo spettro in trasmissione che si osserva in tal
modo contiene informazioni sulle abbondanze presenti nell’atmosfera. Tutta
via\, alcuni fenomeni fisici e chimici possono ostacolare significativamen
te la rilevazione di queste abbondanze. In questa presentazione vengono mo
strati alcuni aspetti dell’osservazione ed analisi di uno spettro in trasm
issione di un’atmosfera esoplanetaria e alcune delle informazioni che è po
ssibile trarre da esso.\n
DTSTART;TZID=Europe/Rome:20220217T150000
DTEND;TZID=Europe/Rome:20220217T160000
SEQUENCE:0
SUMMARY:Seminario online: Valerio Fardella (UNIPA)\, Giovedi` 17 Febbraio o
re 15
URL:http://www.astropa.inaf.it/evento/seminario-online-valerio-fardella-uni
pa-giovedi-17-febbraio-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Valerio Fardella (UNIPA)
\nTitolo: L
’analisi delle atmosfere degli esopianeti. Come e perché.
\nrelazion
e di Laurea triennale\,
\nindirizzo Google Meet: meet.google.com/sxz
-cctp-tsc
\nAbstract:
\nLa composizione chimica dell’atmosfera
di un esopianeta può aiutare a capire quale siano la composizione e\, a v
olte\, l’evoluzione passata dell’esopianeta. L’atmosfera\, se è presente\,
può essere osservata quando il pianeta transita davanti la sua stella. Lo
spettro in trasmissione che si osserva in tal modo contiene informazioni
sulle abbondanze presenti nell’atmosfera. Tuttavia\, alcuni fenomeni fisic
i e chimici possono ostacolare significativamente la rilevazione di queste
abbondanze. In questa presentazione vengono mostrati alcuni aspetti dell’
osservazione ed analisi di uno spettro in trasmissione di un’atmosfera eso
planetaria e alcune delle informazioni che è possibile trarre da esso.
\n
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23193@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220222T100000
DTEND;TZID=Europe/Rome:20220222T123000
SEQUENCE:0
SUMMARY:Riunione Tesi Laurea Zarcone
URL:http://www.astropa.inaf.it/evento/riunione-tesi-laurea-zarcone/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23319@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Ripetizione di tesi magistrale\nLaureanda: Stefania Benanti\nTi
tolo: Studio dell’emissione UV di un CME solare – Possibili estrapolazioni
per la ricerca di CME stellari\nStanza Google meet: https://meet.google.c
om/sxz-cctp-tsc\nAbstract: I CME stellari sono notoriamente difficili da o
sservare\, tanto che a oggi non ci sono CME stellari effettivamente confer
mati ma solo una decina di candidati CME. Mentre identificazione\, osserva
zione e studio dei CME solari è possibile grazie alla risoluzione spaziale
\, in mancanza di quest’ultima è necessario ricorrere a tecniche indirette
per la ricerca dei CME stellari. In particolare si ricorre a tecniche bas
ate sulla ricerca di componenti blueshiftate negli spettri stellari. Tale
ricerca è attualmente effettuata prevalentemente in banda ottica\, tuttavi
a potrebbe essere la banda UV quella più promettente. In questa tesi ho qu
indi scelto un particolare CME solare con lo scopo di studiarne le caratte
ristiche fisiche e determinare l’emissione totale in tutta la banda UV. Av
endo infatti lo spettro totale atteso per il CME\, quanto ricavato in ques
ta tesi può essere riscalato per fare previsioni di quale dovrebbe essere
l’emissione UV di un CME stellare in termini di spettro\, luminosità e dur
ata.\nRelatrice: Costanza Argiroffi
DTSTART;TZID=Europe/Rome:20220314T150000
DTEND;TZID=Europe/Rome:20220314T163000
SEQUENCE:0
SUMMARY:Seminario online: S. Benanti (UNIPA)\, ore 15
URL:http://www.astropa.inaf.it/evento/seminario-online-s-benanti-unipa-ore-
15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRipetizione di tesi magistrale
\nLaureanda: S
tefania Benanti
\nTitolo: Studio dell’emissione UV di un CME solare
– Possibili estrapolazioni per la ricerca di CME stellari
\nStanza G
oogle meet: https://meet.google.com/sxz-cctp-tsc
\nAbstract: I CME s
tellari sono notoriamente difficili da osservare\, tanto che a oggi non ci
sono CME stellari effettivamente confermati ma solo una decina di candida
ti CME. Mentre identificazione\, osservazione e studio dei CME solari è po
ssibile grazie alla risoluzione spaziale\, in mancanza di quest’ultima è n
ecessario ricorrere a tecniche indirette per la ricerca dei CME stellari.
In particolare si ricorre a tecniche basate sulla ricerca di componenti bl
ueshiftate negli spettri stellari. Tale ricerca è attualmente effettuata p
revalentemente in banda ottica\, tuttavia potrebbe essere la banda UV quel
la più promettente. In questa tesi ho quindi scelto un particolare CME sol
are con lo scopo di studiarne le caratteristiche fisiche e determinare l’e
missione totale in tutta la banda UV. Avendo infatti lo spettro totale att
eso per il CME\, quanto ricavato in questa tesi può essere riscalato per f
are previsioni di quale dovrebbe essere l’emissione UV di un CME stellare
in termini di spettro\, luminosità e durata.
\nRelatrice: Costanza A
rgiroffi
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23422@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220321T090000
DTEND;TZID=Europe/Rome:20220321T130000
RDATE;TZID=Europe/Rome:20220322T090000
RDATE;TZID=Europe/Rome:20220323T090000
RDATE;TZID=Europe/Rome:20220324T090000
RDATE;TZID=Europe/Rome:20220325T090000
RDATE;TZID=Europe/Rome:20220328T090000
SEQUENCE:0
SUMMARY:Visite al museo – Light in Astronomy
URL:http://www.astropa.inaf.it/evento/visite-al-museo-light-in-astronomy/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23417@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:26 pax
DTSTART;TZID=Europe/Rome:20220404T150000
DTEND;TZID=Europe/Rome:20220404T170000
SEQUENCE:0
SUMMARY:Visita studenti di Fisica Museo
URL:http://www.astropa.inaf.it/evento/visita-studenti-di-fisica-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n26 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23376@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220405T084500
DTEND;TZID=Europe/Rome:20220407T171500
SEQUENCE:0
SUMMARY:Elezione per rinnovo RSU
URL:http://www.astropa.inaf.it/evento/elezione-per-rinnovo-rsu/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23424@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:9 pax
DTSTART;TZID=Europe/Rome:20220406T163000
DTEND;TZID=Europe/Rome:20220406T180000
SEQUENCE:0
SUMMARY:Visita al museo docenti Erasmus liceo Cassarà
URL:http://www.astropa.inaf.it/evento/visita-al-museo-docenti-erasmus-liceo
-cassara/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n9 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23430@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:7 pax
DTSTART;TZID=Europe/Rome:20220407T110000
DTEND;TZID=Europe/Rome:20220407T124500
SEQUENCE:0
SUMMARY:Visita museo gruppo Beltrano
URL:http://www.astropa.inaf.it/evento/visita-museo-gruppo-beltrano/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n7 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23442@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220426T083000
DTEND;TZID=Europe/Rome:20220429T140000
SEQUENCE:0
SUMMARY:Ricercatori stranieri al museo – no visite – no lavori al museo
URL:http://www.astropa.inaf.it/evento/ricercatori-stranieri-al-museo-no-vis
ite-no-lavori-al-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23462@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220502T090000
DTEND;TZID=Europe/Rome:20220502T130000
SEQUENCE:0
SUMMARY:Gruppo Rosario IARIA
URL:http://www.astropa.inaf.it/evento/gruppo-rosario-iaria/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23444@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:42 + 5
DTSTART;TZID=Europe/Rome:20220513T093000
DTEND;TZID=Europe/Rome:20220513T130000
SEQUENCE:0
SUMMARY:visite al museo pestalozzi cavour
URL:http://www.astropa.inaf.it/evento/visite-al-museo-pestalozzi-cavour/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n42 + 5
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23446@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:24 studenti
DTSTART;TZID=Europe/Rome:20220516T093000
DTEND;TZID=Europe/Rome:20220516T110000
SEQUENCE:0
SUMMARY:Visite al museo pestalozzi cavour
URL:http://www.astropa.inaf.it/evento/visite-al-museo-pestalozzi-cavour-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n24 studenti
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23565@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220517T113000
DTEND;TZID=Europe/Rome:20220517T143000
SEQUENCE:0
SUMMARY:Schiticchio di Donata
URL:http://www.astropa.inaf.it/evento/schiticchio-di-donata/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23537@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:Riunione del gruppo SNR
DTSTART;TZID=Europe/Rome:20220517T150000
DTEND;TZID=Europe/Rome:20220517T170000
SEQUENCE:0
SUMMARY:Riunione SNR
URL:http://www.astropa.inaf.it/evento/riunione-snr/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRiunione del gruppo SNR
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23550@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Seminario in modalita` ibrida\nlink Google meet https://meet.go
ogle.com/sxz-cctp-tsc\nSpeaker: Giacomo Permunian (Universita` di Ferrara)
\nTitolo : La chimica e mineralogia della condrite ordinaria 6A.\nAbstract
: Ordinary chondrites (OCs)\, costituiscono la classe di meteoriti più abb
ondante tra quelle viste cadere (falls) e trovate (finds). Sulla base dell
e loro differenze chimiche\, isotopiche\, mineralogiche e tessiturali (pet
rografiche) sono suddivise in tre gruppi (H\, L\, LL). La possibilità di s
tudiare questi materiali con sempre più dettaglio ha permesso di ampliare
la nostra conoscenza sulla varietà dei materiali nel Sistema Solare e di c
omprendere meglio le condizioni chimico-fisiche della nebulosa solare.\nPr
esenterò lo studio in corso della meteorite COs 6A\, di tipo H\, trovata n
ella provincia di Tata in Marocco\, di cui ho studiato principalmente la p
etrografia (tessitura della roccia) e la composizione mineralogica dei pri
ncipali costituenti (olivina\, Ca-poor pyroxenes e feldspati). Olivine e p
irosseni sono i fondamentali costituenti anche del mantello terrestre (e s
uoi analoghi del sistema solare)\, e sono tra i costituenti più comuni del
le polveri del mezzo inter e circumstellare. Nell’ambito del tirocinio pre
sso l’INAF di Palermo abbiamo usato questi materiali come analoghi di polv
ere inter e circumstellare.
DTSTART;TZID=Europe/Rome:20220519T150000
DTEND;TZID=Europe/Rome:20220519T163000
SEQUENCE:0
SUMMARY:Seminario: Giacomo Permunian (Universita` di Ferrara)
URL:http://www.astropa.inaf.it/evento/seminario-giacomo-permunian-universit
a-di-ferrara/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSeminario in modalita` ibrida
\nlink Google m
eet https://meet.google.com
/sxz-cctp-tsc
\nSpeaker: Giacomo Permunian (Universita` di Ferra
ra)
\nTitolo : La chimica e mineralogia della condrite ordinaria 6A.
\nAbstract: Ordinary chondrites (OCs)\, costituiscono la classe di
meteoriti più abbondante tra quelle viste cadere (falls) e trovate (finds)
. Sulla base delle loro differenze chimiche\, isotopiche\, mineralogiche e
tessiturali (petrografiche) sono suddivise in tre gruppi (H\, L\, LL). La
possibilità di studiare questi materiali con sempre più dettaglio ha perm
esso di ampliare la nostra conoscenza sulla varietà dei materiali nel Sist
ema Solare e di comprendere meglio le condizioni chimico-fisiche della neb
ulosa solare.
\nPresenterò lo studio in corso della meteorite COs 6A\
, di tipo H\, trovata nella provincia di Tata in Marocco\, di cui ho studi
ato principalmente la petrografia (tessitura della roccia) e la composizio
ne mineralogica dei principali costituenti (olivina\, Ca-poor pyroxenes e
feldspati). Olivine e pirosseni sono i fondamentali costituenti anche del
mantello terrestre (e suoi analoghi del sistema solare)\, e sono tra i cos
tituenti più comuni delle polveri del mezzo inter e circumstellare. Nell’a
mbito del tirocinio presso l’INAF di Palermo abbiamo usato questi material
i come analoghi di polvere inter e circumstellare.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23468@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220520T090000
DTEND;TZID=Europe/Rome:20220520T130000
SEQUENCE:0
SUMMARY:Visita istituto comprensivo pirandello Castellammare del Golfo
URL:http://www.astropa.inaf.it/evento/visita-istituto-comprensivo-pirandell
o-castellammare-del-golfo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23541@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Seminario in forma ibrida\,\nindirizzo Google meet: https://mee
t.google.com/sxz-cctp-tsc\nSpeaker: Salvatore Sciortino (INAF)\nTitolo: Th
e Athena predicted PSF and ELSP and their effects on X-ray (stellar) studi
es\nAbtract:\nIn the past 12-18 months improved descriptions of the predic
ted Athena PSF\n(Point Spread Function) and of the predicted Athena/XIFU E
LSF (Extended Line\nSpread Function) have become available and their effec
ts has been investigated by more detailed simulations of WFI and XIFU base
d studies. I will discuss and illustrate the most relevant outcomes of thi
s investigations and their possible effect on (stellar) X-ray studies and
more in general the currently predicted\ncapability (and related limit) of
future Athena observations.
DTSTART;TZID=Europe/Rome:20220523T113000
DTEND;TZID=Europe/Rome:20220523T130000
SEQUENCE:0
SUMMARY:Seminario: S. Sciortino (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-s-sciortino-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSeminario in forma ibrida\,
\nindirizzo Googl
e meet: https://meet.google.com/sxz-cctp-tsc
\nSpeaker: Salvatore Sc
iortino (INAF)
\nTitolo: The Athena predicted PSF and ELSP and their
effects on X-ray (stellar) studies
\nAbtract:
\nIn the past 12
-18 months improved descriptions of the predicted Athena PSF
\n(Point
Spread Function) and of the predicted Athena/XIFU ELSF (Extended Line
\nSpread Function) have become available and their effects has been inve
stigated by more detailed simulations of WFI and XIFU based studies. I wil
l discuss and illustrate the most relevant outcomes of this investigations
and their possible effect on (stellar) X-ray studies and more in general
the currently predicted
\ncapability (and related limit) of future At
hena observations.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23566@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220527T083000
DTEND;TZID=Europe/Rome:20220527T143000
RDATE;TZID=Europe/Rome:20220603T083000
SEQUENCE:0
SUMMARY:Le vie dei tesori
URL:http://www.astropa.inaf.it/evento/le-vie-dei-tesori/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23463@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:33 studenti
DTSTART;TZID=Europe/Rome:20220530T090000
DTEND;TZID=Europe/Rome:20220530T130000
SEQUENCE:0
SUMMARY:Visite al museo e lezione in aula + oculus Einstein (scuola figlia
Giusi)
URL:http://www.astropa.inaf.it/evento/visite-al-museo-scuola-figlia-giusi/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n33 studenti
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23586@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Víctor Almendros Abad (CENTRA\, Faculdade de Ciências
da Universidade de Lisboa\; European Southern Observatory)\nTitle: Milky W
ay’s young substellar population\nindirizzo google meet: https://meet.goog
le.com/sxz-cctp-tsc\nAbstract:\nYoung clusters and star forming regions ar
e home to a large number of substellar objects with masses below the hydro
gen-burning limit at ~0.075 MSun. Most of our knowledge about their popula
tions comes from nearby regions (d < 400 pc)\, where we find consistent fo
rmation rates of 2-5 young brown dwarfs per 10 newborn stars. Brown dwarf
theories\, on the other hand\, predict that high gas or stellar densities\
, as well as the presence of massive OB stars\, may be factors that boost
the incidence of newly formed brown dwarfs with respect to stars. The next
frontier in substellar studies\, therefore\, is the exploration of massiv
e star clusters\, characterized by significantly different star-forming en
vironments than those found in our immediate vicinity. In this contributio
n I will present our deep NIR imaging using the AO-supported instrument HA
WK-I/VLT in Galactic massive clusters RCW 38 and NGC 2244\, complemented b
y the spectroscopic follow-up using KMOS/VLT. We report the most complete
substellar IMFs in the two clusters\, along with the first bona-fide brown
dwarfs beyond 1 kpc\, providing an ideal dataset for a comparison with ne
arby star forming regions. Finally\, I will present our future plans with
two approved JWST programs\, which include the first substellar IMF in a s
tarburst cluster\, and spectroscopic confirmation of first single Jupiter-
mass objects in a nearby star forming region.
DTSTART;TZID=Europe/Rome:20220606T150000
DTEND;TZID=Europe/Rome:20220606T163000
SEQUENCE:0
SUMMARY:Seminario: Víctor Almendros Abad (CENTRA\, Faculdade de Ciências da
Universidade de Lisboa\; European Southern Observatory)\, ore 15
URL:http://www.astropa.inaf.it/evento/seminario-victor-almendros-abad-centr
a-faculdade-de-ciencias-da-universidade-de-lisboa-european-southern-observ
atory-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Víctor Almendros Abad (CENTRA\, Faculdade
de Ciências da Universidade de Lisboa\; European Southern Observatory)
\nTitle: Milky Way’s young substellar population
\nindirizzo goog
le meet: https://meet.google.com/sxz-cctp-tsc
\nAbstract:
\nYou
ng clusters and star forming regions are home to a large number of substel
lar objects with masses below the hydrogen-burning limit at ~0.075 MSun. M
ost of our knowledge about their populations comes from nearby regions (d
< 400 pc)\, where we find consistent formation rates of 2-5 young brown dw
arfs per 10 newborn stars. Brown dwarf theories\, on the other hand\, pred
ict that high gas or stellar densities\, as well as the presence of massiv
e OB stars\, may be factors that boost the incidence of newly formed brown
dwarfs with respect to stars. The next frontier in substellar studies\, t
herefore\, is the exploration of massive star clusters\, characterized by
significantly different star-forming environments than those found in our
immediate vicinity. In this contribution I will present our deep NIR imagi
ng using the AO-supported instrument HAWK-I/VLT in Galactic massive cluste
rs RCW 38 and NGC 2244\, complemented by the spectroscopic follow-up using
KMOS/VLT. We report the most complete substellar IMFs in the two clusters
\, along with the first bona-fide brown dwarfs beyond 1 kpc\, providing an
ideal dataset for a comparison with nearby star forming regions. Finally\
, I will present our future plans with two approved JWST programs\, which
include the first substellar IMF in a starburst cluster\, and spectroscopi
c confirmation of first single Jupiter-mass objects in a nearby star formi
ng region.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23555@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220609T103000
DTEND;TZID=Europe/Rome:20220609T123000
SEQUENCE:0
SUMMARY:Riunione Chinnici
URL:http://www.astropa.inaf.it/evento/riunione-chinnici/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23483@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:SPEAKER: Julien Gressot\, Doctorant FNS – Histoire des techniqu
es et de l’innovation\, Institut d’histoire\nAFFILIATION: Université de Ne
uchâtel (Switzerland)\nTITLE: The Photographic Zenith tube (PZT) of the Ne
uchâtel Observatory: Achievement of time determination or failure of innov
ation?\nABSTRACT: Throughout its existence\, the Neuchâtel Observatory has
sought to be at the forefront of astronomical time determination. In the
mid-20th century\, a technological innovation began to spread in observato
ries with PZTs (Photographic Zenith Tube). The Neuchâtel Observatory was o
ne of the first to obtain this instrument\, the purpose of which was to el
iminate the human factor by automating the time determination and certain
other instrumental errors. PZTs were presented as the most accurate instru
ments of their time\, but their development was soon halted. In this paper
\, we will examine the technical evolution of PZTs\, the reasons why they
became the must-have instrument\, and the explanations for their rapid aba
ndonment.\nGoogle Meet room: https://meet.google.com/sxz-cctp-tsc
DTSTART;TZID=Europe/Rome:20220609T150000
DTEND;TZID=Europe/Rome:20220609T163000
SEQUENCE:0
SUMMARY:Seminario: Julien Gressot (Université de Neuchâtel\, Switzerland)
URL:http://www.astropa.inaf.it/evento/seminario-julien-gressot-universite-d
e-neuchatel-switzerland/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSPEAKER: Julien Gressot\, Doctorant FNS – Histoire
des techniques et de l’innovation\, Institut d’histoire
\nAFFILIATION
: Université de Neuchâtel (Switzerland)
\nTITLE: The Photographic Zen
ith tube (PZT) of the Neuchâtel Observatory: Achievement of time determina
tion or failure of innovation?
\nABSTRACT: Throughout its existence\,
the Neuchâtel Observatory has sought to be at the forefront of astronomic
al time determination. In the mid-20th century\, a technological innovatio
n began to spread in observatories with PZTs (Photographic Zenith Tube). T
he Neuchâtel Observatory was one of the first to obtain this instrument\,
the purpose of which was to eliminate the human factor by automating the t
ime determination and certain other instrumental errors. PZTs were present
ed as the most accurate instruments of their time\, but their development
was soon halted. In this paper\, we will examine the technical evolution o
f PZTs\, the reasons why they became the must-have instrument\, and the ex
planations for their rapid abandonment.
\nGoogle Meet room: https://
meet.google.com/sxz-cctp-tsc
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23558@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220610T103000
DTEND;TZID=Europe/Rome:20220610T123000
SEQUENCE:0
SUMMARY:Riunione Chinnici
URL:http://www.astropa.inaf.it/evento/riunione-chinnici-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23611@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220614T160000
DTEND;TZID=Europe/Rome:20220614T183000
SEQUENCE:0
SUMMARY:Riunione con IEMEST
URL:http://www.astropa.inaf.it/evento/riunione-con-iemest/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23631@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Giusi\; giusi.micela@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220620T090000
DTEND;TZID=Europe/Rome:20220620T140000
LOCATION:Aula
SEQUENCE:0
SUMMARY:UCL-OAPa
URL:http://www.astropa.inaf.it/evento/ucl-oapa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23639@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220620T090000
DTEND;TZID=Europe/Rome:20220620T113000
SEQUENCE:0
SUMMARY:Visita al Museo
URL:http://www.astropa.inaf.it/evento/visita-al-museo-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23610@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:8 pax ref. Sara Bonito
DTSTART;TZID=Europe/Rome:20220621T090000
DTEND;TZID=Europe/Rome:20220622T180000
SEQUENCE:0
SUMMARY:riunione grant rubin lsst al museo
URL:http://www.astropa.inaf.it/evento/riunione-grant-rubin-lsst-al-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n8 pax ref. Sara Bonito
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23630@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Quentin Changeat (UCL)\nTitle: Atmospheric retrievals
in the era of next generation telescopes.\nAbstract: With the recent launc
h of the NASA/ESA/CSA-JWST telescope and the upcoming ESA-Ariel\, we are n
ow entering a new era of exoplanet characterisation. These next-generation
telescopes will revolutionise our understanding of exoplanet atmospheres\
, but the analysis of their observations will be very challenging.\nIn thi
s presentation\, state-of-the-art techniques\, which were thoroughly teste
d to analyse exo-atmospheric data from HST and Spitzer\, will be presented
. We will also explore some of their limitations\, as well as the challeng
es associated with their application to next-generation telescopes.
DTSTART;TZID=Europe/Rome:20220621T150000
DTEND;TZID=Europe/Rome:20220621T163000
SEQUENCE:0
SUMMARY:Seminario: Quentin Changeat (UCL) ore 15
URL:http://www.astropa.inaf.it/evento/seminario-quentin-changeat-ucl-ore-15
/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Quentin Changeat (UCL)
\nTitle: Atmo
spheric retrievals in the era of next generation telescopes.
\nAbstr
act: With the recent launch of the NASA/ESA/CSA-JWST telescope and the upc
oming ESA-Ariel\, we are now entering a new era of exoplanet characterisat
ion. These next-generation telescopes will revolutionise our understanding
of exoplanet atmospheres\, but the analysis of their observations will be
very challenging.
\nIn this presentation\, state-of-the-art techn
iques\, which were thoroughly tested to analyse exo-atmospheric data from
HST and Spitzer\, will be presented. We will also explore some of their li
mitations\, as well as the challenges associated with their application to
next-generation telescopes.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23632@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220622T140000
DTEND;TZID=Europe/Rome:20220622T220000
SEQUENCE:0
SUMMARY:UCL-OAPa
URL:http://www.astropa.inaf.it/evento/ucl-oapa-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23640@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Giovanni Liggio
DESCRIPTION:Lavori di messa in sicurezza cupole astronomiche
DTSTART;TZID=Europe/Rome:20220623T070000
DTEND;TZID=Europe/Rome:20220630T173000
LOCATION:cupole e tetto museo
SEQUENCE:0
SUMMARY:Lavori di messa in sicurezza cupole astronomiche
URL:http://www.astropa.inaf.it/evento/23640/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nLavori di messa in sicurezza cupole astronomiche
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23643@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Visita al Museo (Chinnici) 10 pax
DTSTART;TZID=Europe/Rome:20220624T110000
DTEND;TZID=Europe/Rome:20220624T120000
SEQUENCE:0
SUMMARY:visita al museo
URL:http://www.astropa.inaf.it/evento/visita-al-museo-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nVisita al Museo (Chinnici) 10 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23644@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:visita al museo 5 pax (coniglio)
DTSTART;TZID=Europe/Rome:20220627T090000
DTEND;TZID=Europe/Rome:20220627T130000
SEQUENCE:0
SUMMARY:visita al museo
URL:http://www.astropa.inaf.it/evento/visita-al-museo-5/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nvisita al museo 5 pax (coniglio)
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23482@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220701T080000
DTEND;TZID=Europe/Rome:20220701T130000
SEQUENCE:0
SUMMARY:Visita museo gruppo Sabina
URL:http://www.astropa.inaf.it/evento/visita-museo-gruppo-sabina/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23657@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220705T080000
DTEND;TZID=Europe/Rome:20220705T130000
SEQUENCE:0
SUMMARY:Riprese fotografiche S. Speziale
URL:http://www.astropa.inaf.it/evento/riprese-fotografiche-s-speziale/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23658@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220706T080000
DTEND;TZID=Europe/Rome:20220706T130000
SEQUENCE:0
SUMMARY:Riprese fotografiche S. Speziale
URL:http://www.astropa.inaf.it/evento/riprese-fotografiche-s-speziale-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23659@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:Ref. Laura Daricello
DTSTART;TZID=Europe/Rome:20220707T110000
DTEND;TZID=Europe/Rome:20220707T140000
SEQUENCE:0
SUMMARY:Visita IEMEST
URL:http://www.astropa.inaf.it/evento/visita-iemest/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRef. Laura Daricello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23662@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220725T083000
DTEND;TZID=Europe/Rome:20220725T150000
SEQUENCE:0
SUMMARY:Installazione green studio
URL:http://www.astropa.inaf.it/evento/installazione-green-studio/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23675@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Prova tesi di Edoardo Alaimo (UNIPA)\, seminario in modalita` i
brida\nGoogle meet: https://meet.google.com/sxz-cctp-tsc\n \nTitolo: CHARA
CTERISATION AND MODELLING OF THE UV-VIS-IR TRANSMISSION OF MULTILAYER THIN
FILM FILTERS FOR APPLICATIONS IN HIGH HIGH ENERGY ASTROPHYSICS\nAbstract:
TBD
DTSTART;TZID=Europe/Rome:20220725T150000
DTEND;TZID=Europe/Rome:20220725T163000
SEQUENCE:0
SUMMARY:Seminario: prova tesi Edoardo Alaimo (UNIPA)
URL:http://www.astropa.inaf.it/evento/seminario-prova-tesi-edoardo-alaimo-u
nipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nProva tesi di Edoardo Alaimo (UNIPA)\, seminario in
modalita` ibrida
\nGoogle meet: https://meet.google.com/sxz-cctp-ts
c
\n
\nTitolo: CHARACTERISATION AND MODELLING OF THE UV-VIS-I
R TRANSMISSION OF MULTILAYER THIN FILM FILTERS FOR APPLICATIONS IN HIGH HI
GH ENERGY ASTROPHYSICS
\nAbstract: TBD
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23866@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:totale 20 pax + 4 guide amici dei musei
DTSTART;TZID=Europe/Rome:20220729T183000
DTEND;TZID=Europe/Rome:20220729T234500
SEQUENCE:0
SUMMARY:RESTART Visite notturne al Museo della Specola
URL:http://www.astropa.inaf.it/evento/restart-visite-notturne-al-museo-dell
a-specola/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\ntotale 20 pax + 4 guide amici dei musei
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23797@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Visita Museo Jordie Sans Forcada\n7 pax
DTSTART;TZID=Europe/Rome:20220901T093000
DTEND;TZID=Europe/Rome:20220901T110000
SEQUENCE:0
SUMMARY:Visita Museo Jordie Sans Forcada
URL:http://www.astropa.inaf.it/evento/visita-museo-jordie-sans-forcada/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nVisita Museo Jordie Sans Forcada
\n7 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23804@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Aiello ore 9\n
DTSTART;TZID=Europe/Rome:20220906T090000
DTEND;TZID=Europe/Rome:20220906T100000
SEQUENCE:0
SUMMARY:Visita museo 2 persone: Aiello
URL:http://www.astropa.inaf.it/evento/visita-museo-3-persone-alienor-barbie
r/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nAiello ore 9
\n
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23803@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Seminario in forma ibrida\nIndirizzo Google meet: https://meet.
google.com/sxz-cctp-tsc\nSpeaker: R. Giuffrida (UNIPA)\nTitolo: The supern
ova remnant SN 1006 as a Galactic particle accelerator\nAbstract:\nThe ori
gin of cosmic-rays is an open issue of high-energy astrophysics. Supernova
remnants are expected to be the main source of Galactic cosmic rays up to
energies of about 3 PeV\, provided that they transfer a significant fract
ion of their kinetic energy to the particles (∼ 10%). In particular\, the
loss of such a large fraction of energy is predicted to alter the shock dy
namics by enhancing the shock compression ratio above the canonical value
of 4 (shock modification). The bilateral supernova remnant SN 1006 is an i
deal target to study shock modification because of its evolution in a fair
ly uniform environment. SN 1006 shows bright synchrotron X-ray emission fr
om ultrarelativistic electrons accelerated at the shock front in its north
eastern and southwestern limbs. If efficient hadron acceleration occurs in
these regions\, we should observe shock modification therein. We performe
d a spatially resolved spectral analysis of Chandra and XMM-Newton observa
tions of SN 1006 by selecting narrow regions between the shock front and t
he contact discontinuity and measuring the density of the X-ray emitting p
lasma. Our results show an increase of the compression ratio from the char
acteristic value of 4\, in thermal limb\, up to ∼ 7 in nonthermal limbs\,
i.e. in regions where the ambient magnetic field is almost parallel to the
shock velocity. We conclude that an efficient particle acceleration cause
s shock modification in quasi-parallel shocks in SN 1006. By comparing our
results with state-of-the-art models\, we find that SN 1006 is transferri
ng a significant fraction of its kinetic energy to hadrons. The inferred v
alues of compression ratios and cosmic ray slopes are consistent with thos
e expected for modified shocks when the effects of the postcursor are incl
uded.
DTSTART;TZID=Europe/Rome:20220906T150000
DTEND;TZID=Europe/Rome:20220906T163000
SEQUENCE:0
SUMMARY:Seminario: R. Giuffrida (UNIPA)
URL:http://www.astropa.inaf.it/evento/seminario-r-giuffrida-unipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSeminario in forma ibrida
\nIndirizzo Google
meet: https://meet.google.com/sxz-cctp-tsc
\nSpeaker: R. Giuffrida (
UNIPA)
\nTitolo: The supernova remnant SN 1006 as a Galactic particle
accelerator
\nAbstract:
\nThe origin of cosmic-rays is an open
issue of high-energy astrophysics. Supernova remnants are expected to be t
he main source of Galactic cosmic rays up to energies of about 3 PeV\, pro
vided that they transfer a significant fraction of their kinetic energy to
the particles (∼ 10%). In particular\, the loss of such a large fraction
of energy is predicted to alter the shock dynamics by enhancing the shock
compression ratio above the canonical value of 4 (shock modification). The
bilateral supernova remnant SN 1006 is an ideal target to study shock mod
ification because of its evolution in a fairly uniform environment. SN 100
6 shows bright synchrotron X-ray emission from ultrarelativistic electrons
accelerated at the shock front in its northeastern and southwestern limbs
. If efficient hadron acceleration occurs in these regions\, we should obs
erve shock modification therein. We performed a spatially resolved spectra
l analysis of Chandra and XMM-Newton observations of SN 1006 by selecting
narrow regions between the shock front and the contact discontinuity and m
easuring the density of the X-ray emitting plasma. Our results show an inc
rease of the compression ratio from the characteristic value of 4\, in the
rmal limb\, up to ∼ 7 in nonthermal limbs\, i.e. in regions where the ambi
ent magnetic field is almost parallel to the shock velocity. We conclude t
hat an efficient particle acceleration causes shock modification in quasi-
parallel shocks in SN 1006. By comparing our results with state-of-the-art
models\, we find that SN 1006 is transferring a significant fraction of i
ts kinetic energy to hadrons. The inferred values of compression ratios an
d cosmic ray slopes are consistent with those expected for modified shocks
when the effects of the postcursor are included.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23844@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Aula: Teleconferenza
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220907T113000
DTEND;TZID=Europe/Rome:20220907T123000
SEQUENCE:0
SUMMARY:Telecon Sara\, Loredana\, Jesus\, Paolo (remoto)
URL:http://www.astropa.inaf.it/evento/telecon-sara-loredana-jesus-paolo-rem
oto/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23862@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:visita museo ARS 4 pax
DTSTART;TZID=Europe/Rome:20220908T100000
DTEND;TZID=Europe/Rome:20220908T111500
SEQUENCE:0
SUMMARY:visita museo ARS 4 pax
URL:http://www.astropa.inaf.it/evento/visita-museo-ars-4-pax/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nvisita museo ARS 4 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23863@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Totale 20 pax + 4 guide Amici dei Musei
DTSTART;TZID=Europe/Rome:20220909T183000
DTEND;TZID=Europe/Rome:20220909T234500
SEQUENCE:0
SUMMARY:Restart e visite notturne al museo della Specola
URL:http://www.astropa.inaf.it/evento/restart-e-visite-notturne-al-museo-de
lla-specola/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nTotale 20 pax + 4 guide Amici dei Musei
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23857@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:La collega di INAF-OAR Tiziana Macaluso sarà in osservatorio pe
r effettuare il restauro di alcune fotografie storiche e avrà bisogno di s
pazi più ampi di una normale scrivania per svolgere la sua attività: per q
uesto motivo lavorerà nei locali del museo per tutta la settimana.
DTSTART;TZID=Europe/Rome:20220912T090000
DTEND;TZID=Europe/Rome:20220916T170000
SEQUENCE:0
SUMMARY:Laboratorio di restauro fotografico
URL:http://www.astropa.inaf.it/evento/laboratorio-di-restauro-fotografico/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nLa collega di INAF-OAR Tiziana Macaluso sarà in oss
ervatorio per effettuare il restauro di alcune fotografie storiche e avrà
bisogno di spazi più ampi di una normale scrivania per svolgere la sua att
ività: per questo motivo lavorerà nei locali del museo per tutta la settim
ana.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23805@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Seminario in forma ibrida\nIndirizzo Google Meet: https://meet.
google.com/sxz-cctp-tsc\nSpeaker: Vincenzo Sapienza (UNIPA)\nTitolo: A spa
tially resolved study of hard X-ray emission in Kepler’s SNR: indications
of different regimes of particle acceleration\nAbstract:\nL’emissione di S
incrotrone nei raggi X proveniente da resti di supernova (SNR) giovani è u
n potente strumento diagnostico per studiare la popolazione di elettroni a
ltamente energetici accelerati al fronte di shock oltre che per studiare i
l processo di accelerazione stesso.\nIn questo lavoro abbiamo eseguito un’
analisi spettrale spazialmente risolta di osservazioni NuSTAR e XMM-Newton
del giovane SNR di Keplero\, con lo scopo di studiare in dettaglio la sua
emissione non termica nei raggi X duri.\nGli spettri sono stato analizzat
i adottando un modello di radiazione di sincrotrone in un regime in cui l’
energia massima degli elettroni è limitata dalle perdite radiative\, in mo
do da vincolare la dipendenza dell’energia di cutoff del sincrotrone dalla
velocità del fronte di shock.\nAbbiamo identificato due diversi regimi di
accelerazione di particelle.\nA nord\, dove lo shock sta interagendo con
un mezzo circumstellare denso\, abbiamo trovato una accelerazione più effi
ciente che a sud\, dove la velocità del fronte di shock è più alta e non c
i sono segni di interazione tra shock e un mezzo circumstellare denso.\nI
nostri risultati suggeriscono un’efficienza maggiore in regioni dove l’int
erazione tra shock e mezzo circumstellare genera un campo magnetico turbol
ento ed amplificato.\nCombinando lo spettro nei raggi X duri con osservazi
oni radio e gamma del SNR di Keplero\, abbiamo modellato la distribuzione
dell’energia spettrale (SED). Alla luce dei nostri risultati proponiamo ch
e l’emissione gamma osservata sia principalmente adronica (associata a pro
toni ultrarelativistici)\, e che origini dalla parte nord del resto.
DTSTART;TZID=Europe/Rome:20220914T150000
DTEND;TZID=Europe/Rome:20220914T163000
SEQUENCE:0
SUMMARY:Seminario: Vincenzo Sapienza (UNIPA)
URL:http://www.astropa.inaf.it/evento/seminario-vincenzo-sapienza-unipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSeminario in forma ibrida
\nIndirizzo Google
Meet: https://meet.google.com/sxz-cctp-tsc
\nSpeaker: Vincenzo Sapie
nza (UNIPA)
\nTitolo: A spatially resolved study of hard X-ray emiss
ion in Kepler’s SNR: indications of different regimes of particle accelera
tion
\nAbstract:
\nL’emissione di Sincrotrone nei raggi X prove
niente da resti di supernova (SNR) giovani è un potente strumento diagnost
ico per studiare la popolazione di elettroni altamente energetici accelera
ti al fronte di shock oltre che per studiare il processo di accelerazione
stesso.
\nIn questo lavoro abbiamo eseguito un’analisi spettrale spaz
ialmente risolta di osservazioni NuSTAR e XMM-Newton del giovane SNR di Ke
plero\, con lo scopo di studiare in dettaglio la sua emissione non termica
nei raggi X duri.
\nGli spettri sono stato analizzati adottando un m
odello di radiazione di sincrotrone in un regime in cui l’energia massima
degli elettroni è limitata dalle perdite radiative\, in modo da vincolare
la dipendenza dell’energia di cutoff del sincrotrone dalla velocità del fr
onte di shock.
\nAbbiamo identificato due diversi regimi di acceleraz
ione di particelle.
\nA nord\, dove lo shock sta interagendo con un m
ezzo circumstellare denso\, abbiamo trovato una accelerazione più efficien
te che a sud\, dove la velocità del fronte di shock è più alta e non ci so
no segni di interazione tra shock e un mezzo circumstellare denso.
\n
I nostri risultati suggeriscono un’efficienza maggiore in regioni dove l’i
nterazione tra shock e mezzo circumstellare genera un campo magnetico turb
olento ed amplificato.
\nCombinando lo spettro nei raggi X duri con o
sservazioni radio e gamma del SNR di Keplero\, abbiamo modellato la distri
buzione dell’energia spettrale (SED). Alla luce dei nostri risultati propo
niamo che l’emissione gamma osservata sia principalmente adronica (associa
ta a protoni ultrarelativistici)\, e che origini dalla parte nord del rest
o.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23843@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speakers1 Alessandro Salvatore Tramuto\nTitolo1: Photometric cl
assification of variable young stellar objects and Optimization of the Rub
in LSST Observing Strategy\nAbstract1: \nLa presentazione consiste nella c
lassificazione\, mediante il confronto delle rispettive curve di luce (LCs
)\, di oggetti stellari giovani (YSOs) caratterizzati da variabilità su di
versi tempi scala. Inoltre\, vengono usate queste stesse LCs come base per
uno studio sull’ottimizzazione della strategia osservativa relativa alla
Legacy Survey of Space and Time del telescopio Vera C. Rubin\, al fine di
trovare la cadenza di\ncampionamento più efficace per ricreare le LCs nei
vari tempi scala considerati.\nDopo aver descritto rapidamente il processo
di accrescimento per le YSOs\, vengono date informazioni in merito al tel
escopio Vera C. Rubin e al funzionamento della survey. Segue la classifica
zione fotometrica delle YSOs\, con il relativo studio sull’ottimizzazione
della strategia osservativa\, per concludere con la visione\ndi una LC ric
avata da dati simulati\, ottenuti dalla Rubin Science Platform\, l’infrast
ruttura Rubin usata per l’analisi dati dei futuri dati Rubin.\n———————————
—————————————————————————–\nSpeaker2: Simona Caserta\nTitolo2: FORMAZIONE
PLANETARIA: FORMAZIONE DEI PIANETI TERRESTRI\nAbstract2: \nLa presentazion
e mira a descrivere il processo di formazione di un pianeta di tipo terres
tre in accordo allo scenario di accrescimento sequenziale.\nLe domande a c
ui si vuole dare una risposta sono:\nCome piccole particelle solide cresco
no all’interno del disco protoplanetario\, sede di formazione planetaria?
\nCome si formano i pianeti terrestri?\nDopo aver illustrato le caratteris
tiche principali del disco protoplanetario\, si procede alla descrizione d
el processo di crescita dei granelli di polvere in planetesimi.\nSuccessiv
amente\, viene descritta la crescita dei planetesimi in protopianeti\, spi
egando il fenomeno della focalizzazione gravitazionale e mostrando i due p
rincipali modi di crescita: crescita ordinata e crescita runaway. Per most
rare l’evoluzione dei planetesimi\, viene realizzato un modello numerico\,
il metodo diretto\ndegli N-corpi\, che consiste nel risolvere le equazion
i del moto associate agli N planetesimi per integrazione. Infine\, viene d
escritta la fine della crescita dei protopianeti e l’assemblaggio dei pian
eti terrestri\, elencando i\nrisultati ottenuti da simulazioni numeriche.
DTSTART;TZID=Europe/Rome:20220915T150000
DTEND;TZID=Europe/Rome:20220915T163000
SEQUENCE:0
SUMMARY:Seminario: presentazione della tesi di studenti UNIPA: Tramuto e Ca
serta
URL:http://www.astropa.inaf.it/evento/seminario-presentazione-della-tesi-di
-studenti-unipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeakers1 Alessandro Salvatore Tramuto
\nTitol
o1: Photometric classification of variable young stellar objects and Optim
ization of the Rubin LSST Observing Strategy
\nAbstract1:
\nLa presentazione consiste nella classificazione\, mediante il c
onfronto delle rispettive curve di luce (LCs)\, di oggetti stellari giovan
i (YSOs) caratterizzati da variabilità su diversi tempi scala. Inoltre\, v
engono usate queste stesse LCs come base per uno studio sull’ottimizzazion
e della strategia osservativa relativa alla Legacy Survey of Space and Tim
e del telescopio Vera C. Rubin\, al fine di trovare la cadenza di
\nc
ampionamento più efficace per ricreare le LCs nei vari tempi scala conside
rati.
\nDopo aver descritto rapidamente il processo di accrescimento
per le YSOs\, vengono date informazioni in merito al telescopio Vera C. Ru
bin e al funzionamento della survey. Segue la classificazione fotometrica
delle YSOs\, con il relativo studio sull’ottimizzazione della strategia os
servativa\, per concludere con la visione
\ndi una LC ricavata da dat
i simulati\, ottenuti dalla Rubin Science Platform\, l’infrastruttura Rubi
n usata per l’analisi dati dei futuri dati Rubin.
\n————————————————
————————————————————–
\nSpeaker2: Simona Caserta
\nTitolo2: FOR
MAZIONE PLANETARIA: FORMAZIONE DEI PIANETI TERRESTRI
\nAbstract2:
\nLa presentazione mira a descrivere il processo d
i formazione di un pianeta di tipo terrestre in accordo allo scenario di a
ccrescimento sequenziale.
\nLe domande a cui si vuole dare una rispos
ta sono:
\nCome piccole particelle solide crescono all’interno del di
sco protoplanetario\, sede di formazione planetaria?
\nCome si forman
o i pianeti terrestri?
\nDopo aver illustrato le caratteristiche prin
cipali del disco protoplanetario\, si procede alla descrizione del process
o di crescita dei granelli di polvere in planetesimi.
\nSuccessivamen
te\, viene descritta la crescita dei planetesimi in protopianeti\, spiegan
do il fenomeno della focalizzazione gravitazionale e mostrando i due princ
ipali modi di crescita: crescita ordinata e crescita runaway. Per mostrare
l’evoluzione dei planetesimi\, viene realizzato un modello numerico\, il
metodo diretto
\ndegli N-corpi\, che consiste nel risolvere le equazi
oni del moto associate agli N planetesimi per integrazione. Infine\, viene
descritta la fine della crescita dei protopianeti e l’assemblaggio dei pi
aneti terrestri\, elencando i
\nrisultati ottenuti da simulazioni num
eriche.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23893@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220919T090000
DTEND;TZID=Europe/Rome:20220919T130000
LOCATION:Museo
SEQUENCE:0
SUMMARY:Concorso dottorato
URL:http://www.astropa.inaf.it/evento/23893/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23894@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220919T160000
DTEND;TZID=Europe/Rome:20220919T190000
LOCATION:Museo
SEQUENCE:0
SUMMARY:Concorso dottorato
URL:http://www.astropa.inaf.it/evento/concorso-dottorato/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23895@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220920T090000
DTEND;TZID=Europe/Rome:20220920T130000
LOCATION:Museo
SEQUENCE:0
SUMMARY:Concorso dottorato
URL:http://www.astropa.inaf.it/evento/concorso-dottorato-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23880@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20220920T140000
DTEND;TZID=Europe/Rome:20220920T170000
SEQUENCE:0
SUMMARY:Telecon Serena
URL:http://www.astropa.inaf.it/evento/telecon-serena-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23795@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:GIOVANNI XXIII I.C. TERRASINI\nVisita per delegazione docenti s
tranieri\, nell’ambito del Progetto Erasmus+ “Outdoor learning – Leading t
he Curriculum”
DTSTART;TZID=Europe/Rome:20220921T090000
DTEND;TZID=Europe/Rome:20220921T130000
SEQUENCE:0
SUMMARY:Visita al Museo
URL:http://www.astropa.inaf.it/evento/visita-al-museo-6/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nGIOVANNI XXIII I.C
. TERRASINI
\nVisita per delegazione docenti stranieri\, ne
ll’ambito del Progetto Erasmus+ “Outdoor learning – Leading the Curriculum
”
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23928@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:polizia boccadifalco\n20 pax – guarcello
DTSTART;TZID=Europe/Rome:20220923T090000
DTEND;TZID=Europe/Rome:20220923T130000
SEQUENCE:0
SUMMARY:Visita museo della specola
URL:http://www.astropa.inaf.it/evento/visita-museo-della-specola/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\npolizia boccadifalco
\n20 pax – guarcello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23796@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Visita Museo Rossella Angelica Baldi
DTSTART;TZID=Europe/Rome:20220926T090000
DTEND;TZID=Europe/Rome:20220926T130000
SEQUENCE:0
SUMMARY:Visita Museo Rossella Angelica Baldi
URL:http://www.astropa.inaf.it/evento/visita-museo-rossella-angelica-baldi/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nVisita Museo Rossella Angelica Baldi
\n
HTML>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23845@www.astropa.inaf.it
DTSTAMP:20240329T140514Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Marco Barbera\; 3346399413
DESCRIPTION:Riunione programmatica del progetto Athena X-IFU con l’agenzia
spaziale francese CNES.
DTSTART;TZID=Europe/Rome:20221004T093000
DTEND;TZID=Europe/Rome:20221004T163000
SEQUENCE:0
SUMMARY:Riunione progetto Athena
URL:http://www.astropa.inaf.it/evento/riunione-progetto-athena/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRiunione programmatica del progetto Athena X-IFU co
n l’agenzia spaziale francese CNES.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23993@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221006T090000
DTEND;TZID=Europe/Rome:20221006T110000
SEQUENCE:0
SUMMARY:Riunione Direttore – Servizio Museo
URL:http://www.astropa.inaf.it/evento/riunione-direttore-servizio-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23989@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Indirizzo Google Meet: https://meet.google.com/jsc-eufh-iek\nSp
eaker: Mauro Sansica (UNIPA)\nTitolo: ANALISI IN BANDA X DEI BRILLAMENTI D
ELLA STELLA T TAURI TW HYA\nAbstract:\nLe T Tauri Stars sono stelle di pic
cola massa principalmente localizzate in regioni di formazione stellare e
responsabili di una forte emissione di raggi X causata da una elevata atti
vità magnetica. La principale componente di emissione X è legata ai brilla
menti che sono in grado di scaldare il plasma coronale fino a temperature
superiori ai 100 MK. A questa categoria di stelle appartengono le Classica
l T Tauri Stars\, dotate di un disco di accrescimento che\, interagendo co
n le strutture magnetiche stellari\, sembrrerebbe influire sull’attività m
agnetica.\nPer comprendere meglio le proprietà magnetiche e coronali di un
a stella con accrescimento\, presento in questo lavoro di tesi uno studio
sui brillamenti X della stella TW Hydrae\, rivelati durante i 537 ks di os
servazione effettuata con il telescopio spaziale Chandra con al fuoco il r
ivelatore ACIS-S e l’utilizzo del grating HETG.\nAttraverso lo studio spet
troscopico risolto in tempo dell’emissione X dei brillamenti più intensi h
o avuto modo di risalire alle dimensioni delle loop generate e all’intensi
tà dei campi magnetici necessari per confinare il plasma.\nL’analisi della
frequenza e della distribuzione energetica dei brillamenti su una stella
a distanza così ridotta dal Sistema Solare come TW Hya\, permetterà di evi
denziare eventi poco intensi che in generale gli studi su vaste aree di fo
rmazione stellare a distanze notevoli non riescono a rivelare.
DTSTART;TZID=Europe/Rome:20221006T150000
DTEND;TZID=Europe/Rome:20221006T163000
SEQUENCE:0
SUMMARY:Seminario: prova tesi di laurea M. Sansica (UNIPA)
URL:http://www.astropa.inaf.it/evento/seminario-prova-tesi-di-laurea-m-sans
ica-unipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nIndirizzo Google Meet: https://meet.google.com/jsc-
eufh-iek
\nSpeaker: Mauro Sansica (UNIPA)
\nTitolo: ANALISI IN
BANDA X DEI BRILLAMENTI DELLA STELLA T TAURI TW HYA
\nAbstract:
\nLe T Tauri Stars sono stelle di piccola massa principalmente localizzate
in regioni di formazione stellare e responsabili di una forte emissione d
i raggi X causata da una elevata attività magnetica. La principale compone
nte di emissione X è legata ai brillamenti che sono in grado di scaldare i
l plasma coronale fino a temperature superiori ai 100 MK. A questa categor
ia di stelle appartengono le Classical T Tauri Stars\, dotate di un disco
di accrescimento che\, interagendo con le strutture magnetiche stellari\,
sembrrerebbe influire sull’attività magnetica.
\nPer comprendere megl
io le proprietà magnetiche e coronali di una stella con accrescimento\, pr
esento in questo lavoro di tesi uno studio sui brillamenti X della stella
TW Hydrae\, rivelati durante i 537 ks di osservazione effettuata con il te
lescopio spaziale Chandra con al fuoco il rivelatore ACIS-S e l’utilizzo d
el grating HETG.
\nAttraverso lo studio spettroscopico risolto in tem
po dell’emissione X dei brillamenti più intensi ho avuto modo di risalire
alle dimensioni delle loop generate e all’intensità dei campi magnetici ne
cessari per confinare il plasma.
\nL’analisi della frequenza e della
distribuzione energetica dei brillamenti su una stella a distanza così rid
otta dal Sistema Solare come TW Hya\, permetterà di evidenziare eventi poc
o intensi che in generale gli studi su vaste aree di formazione stellare a
distanze notevoli non riescono a rivelare.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23806@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:64 pax
DTSTART;TZID=Europe/Rome:20221007T090000
DTEND;TZID=Europe/Rome:20221007T140000
RDATE;TZID=Europe/Rome:20221014T090000
SEQUENCE:0
SUMMARY:Visite al museo Vie dei Tesori dalle 9 alle 14
URL:http://www.astropa.inaf.it/evento/visite-al-museo-vie-dei-tesori-dalle-
9-alle-14/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n64 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24047@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:30 pax
DTSTART;TZID=Europe/Rome:20221012T093000
DTEND;TZID=Europe/Rome:20221012T123000
SEQUENCE:0
SUMMARY:visita museo – studenti Vitale
URL:http://www.astropa.inaf.it/evento/visita-museo-studenti-vitale/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n30 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23967@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:2 pax
DTSTART;TZID=Europe/Rome:20221017T090000
DTEND;TZID=Europe/Rome:20221017T130000
SEQUENCE:0
SUMMARY:Visita museo Fichera
URL:http://www.astropa.inaf.it/evento/visita-museo-fichera/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n2 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24048@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Liceo Croce
DTSTART;TZID=Europe/Rome:20221025T100000
DTEND;TZID=Europe/Rome:20221025T124500
SEQUENCE:0
SUMMARY:visita museo liceo croce
URL:http://www.astropa.inaf.it/evento/visita-museo-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nLiceo Croce
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24099@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221026T150000
DTEND;TZID=Europe/Rome:20221026T170000
SEQUENCE:0
SUMMARY:visita museo due bambini + genitori
URL:http://www.astropa.inaf.it/evento/visita-museo-due-bambini-genitori/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24149@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221027T143000
DTEND;TZID=Europe/Rome:20221027T193000
SEQUENCE:0
SUMMARY:Concorso INAF
URL:http://www.astropa.inaf.it/evento/concorso-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
X-TAGS;LANGUAGE=it-IT:Commissione concorso
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24192@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221103T110000
DTEND;TZID=Europe/Rome:20221103T130000
SEQUENCE:0
SUMMARY:Consiglio di Struttura
URL:http://www.astropa.inaf.it/evento/consiglio-di-struttura-8/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24157@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221104T150000
DTEND;TZID=Europe/Rome:20221104T170000
SEQUENCE:0
SUMMARY:Visita museo 7 pax Misilmeri – Chinnici
URL:http://www.astropa.inaf.it/evento/visita-museo-7-pax-misilmeri-chinnici
/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24049@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:40 studenti\nprimo turno 9.30\nsecondo turno 11\n
DTSTART;TZID=Europe/Rome:20221107T090000
DTEND;TZID=Europe/Rome:20221107T130000
SEQUENCE:0
SUMMARY:visita museo istituto paritario trinacria
URL:http://www.astropa.inaf.it/evento/visita-museo-scuola-media-trinacria/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n40 studenti
\nprimo turno 9.30
\nsecond
o turno 11
\n
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24162@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Stanza Google meet: meet.google.com/sxz-cctp-tsc\nSpeaker: Giul
iana Cosentino (Space\, Earth and Environment Department\, Chalmers Univer
sity of Technology\, SE)\nTitle: Feedback from Supernova Remnants: trigger
ing Star Formation in the ISM\nAbstract: Supernova remnants (SNRs) drive l
arge-scale shocks that locally enhance the density of the surrounding mate
rial but also inject vast amounts of energy and momentum that largely pert
urb and disperse the Interstellar Medium (ISM).\nThe interplay between the
se two effects is considered paramount in regulating the star formation ef
ficiency in galaxies. However\, how SNRs affect the physical conditions of
the ISM is not well constrained from an observational point of view.\nIn
this talk\, I will present our work aimed to address this question.\nI wil
l show our study of the large scale shock triggered by the SNR W44 on the
molecular cloud G034. I will show how the shock\, probed by Silicon Monoxi
de (SiO) and observed with ALMA\, enhances the density of the processed ga
s to values compatible with those required for massive star formation and
has helped to shape the cloud. I will also present our exploratory large s
ingle-dish\nobserving program SHREC\, aimed to observe the molecular shock
tracer\nSiO(2-1) toward a sample of 30 SNRs known to be interacting with
molecular clouds. I will introduce the aim and technical aspects of SHREC
and present the first results obtained toward the SNRs IC443.\nIC443 is a
well known SNR\, expanding into and interacting with a nearby toroidal mol
ecular cloud. Toward the major site of interaction\, known as clump G\, we
estimate the mass of the shocked gas to be 100 Msun.\nThe shock driven by
IC443 into this material enhances its density by a factor >10\, to value
consistent with those required to ignite star formation. Finally\, we esti
mate that between 35-50% of the momentum injected by IC443 is transferred
to the nearby molecular material. Our work therefore indicates that the mo
lecular ISM is an important carrier of the SNR momentum and that the SNR-m
olecular cloud interaction play a crucial role in the regulating star form
ation in galaxies.
DTSTART;TZID=Europe/Rome:20221108T150000
DTEND;TZID=Europe/Rome:20221108T163000
SEQUENCE:0
SUMMARY:Seminario: Giuliana Cosentino (Chalmers University of Technology\,
SE)\, Aula\, ore 15
URL:http://www.astropa.inaf.it/evento/seminario-giuliana-cosentino-chalmers
-university-of-technology-se-aula-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nStanza Google meet: meet.google.com/sxz-cctp-tsc
\nSpeaker: Giuliana Cosentino (Space\, Earth and Environment Departmen
t\, Chalmers University of Technology\, SE)
\nTitle: Feedback from S
upernova Remnants: triggering Star Formation in the ISM
\nAbstract:
Supernova remnants (SNRs) drive large-scale shocks that locally enhance th
e density of the surrounding material but also inject vast amounts of ener
gy and momentum that largely perturb and disperse the Interstellar Medium
(ISM).
\nThe interplay between these two effects is considered paramo
unt in regulating the star formation efficiency in galaxies. However\, how
SNRs affect the physical conditions of the ISM is not well constrained fr
om an observational point of view.
\nIn this talk\, I will present ou
r work aimed to address this question.
\nI will show our study of the
large scale shock triggered by the SNR W44 on the molecular cloud G034. I
will show how the shock\, probed by Silicon Monoxide (SiO) and observed w
ith ALMA\, enhances the density of the processed gas to values compatible
with those required for massive star formation and has helped to shape the
cloud. I will also present our exploratory large single-dish
\nobser
ving program SHREC\, aimed to observe the molecular shock tracer
\nSi
O(2-1) toward a sample of 30 SNRs known to be interacting with molecular c
louds. I will introduce the aim and technical aspects of SHREC and present
the first results obtained toward the SNRs IC443.
\nIC443 is a well
known SNR\, expanding into and interacting with a nearby toroidal molecula
r cloud. Toward the major site of interaction\, known as clump G\, we esti
mate the mass of the shocked gas to be 100 Msun.
\nThe shock driven b
y IC443 into this material enhances its density by a factor >10\, to value
consistent with those required to ignite star formation. Finally\, we est
imate that between 35-50% of the momentum injected by IC443 is transferred
to the nearby molecular material. Our work therefore indicates that the m
olecular ISM is an important carrier of the SNR momentum and that the SNR-
molecular cloud interaction play a crucial role in the regulating star for
mation in galaxies.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24200@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221111T100000
DTEND;TZID=Europe/Rome:20221111T180000
SEQUENCE:0
SUMMARY:Riprese documentario MediaInaf
URL:http://www.astropa.inaf.it/evento/riprese-documentario-mediainaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24183@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Stanza Google Meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Marcell Tessenyi (BSS Italia)\nTitolo: Mauve and Twinkle: UV and infr
ared satellites delivered through a new model\nAbstract:\nMauve and Twinkl
e are part of a new family of satellites from Blue Skies Space that use th
e latest commercial space industry developments to deliver scientific miss
ions on vastly accelerated timescales\, setting a new pace for science dis
covery.\nMauve is a low-Earth orbit (LEO) small satellite containing a UV
spectrometer and a 15cm class telescope. It is designed to monitor the act
ivity of nearby stars\, with a particular focus on M-dwarfs that might hos
t habitable zone planets. The construction begins this year with partners
C3S and ISISpace\, for a planned launch in early 2024. Twinkle is a larger
LEO satellite carrying a 0.45m telescope and an infrared spectrometer wit
h a simultaneous wavelength coverage from 0.5 to 4.5μm. It is designed to
detect the composition of atmospheres of exoplanets orbiting bright stars\
, as well as solar system objects such as comets and asteroids. The satell
ite\, expected to launch in late 2024\, is based on a high-heritage platfo
rm from Airbus and an instrument by ABB Canada. Both satellites will provi
de scientific data highly complementary to existing and upcoming exoplanet
related space and ground-based observatories\, including NASA/ESA/CSA’s J
ames Webb Space Telescope and ESO’s Extremely Large Telescope.\nBlue Skies
Space is able to deliver Mauve and Twinkle thanks to the substantial tran
sformations currently on-going in the space sector in Europe and beyond. B
lue Skies Space Italia S.R.L. was set up this year to leverage the capabil
ities and expertise of the Italian science and technology community and he
lp coordinate European science\, technology and funding activities.
DTSTART;TZID=Europe/Rome:20221114T150000
DTEND;TZID=Europe/Rome:20221114T160000
SEQUENCE:0
SUMMARY:Seminario: Marcell Tessenyi (BSS Italia) \, 14 Novembre ore 15.00
URL:http://www.astropa.inaf.it/evento/seminario-marcell-tessenyi-ucl-14-nov
embre-ore-15-00/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nStanza Google Meet: https://meet.google.com/sxz-cct
p-tsc
\nSpeaker: Marcell Tessenyi (BSS Italia)
\nTitolo: Mauv
e and Twinkle: UV and infrared satellites delivered through a new model
\nAbstract:
\nMauve and Twinkle are part of a new family of sate
llites from Blue Skies Space that use the latest commercial space industry
developments to deliver scientific missions on vastly accelerated timesca
les\, setting a new pace for science discovery.
\nMauve is a low-Ear
th orbit (LEO) small satellite containing a UV spectrometer and a 15cm cla
ss telescope. It is designed to monitor the activity of nearby stars\, wit
h a particular focus on M-dwarfs that might host habitable zone planets. T
he construction begins this year with partners C3S and ISISpace\, for a pl
anned launch in early 2024. Twinkle is a larger LEO satellite carrying a 0
.45m telescope and an infrared spectrometer with a simultaneous wavelength
coverage from 0.5 to 4.5μm. It is designed to detect the composition of a
tmospheres of exoplanets orbiting bright stars\, as well as solar system o
bjects such as comets and asteroids. The satellite\, expected to launch in
late 2024\, is based on a high-heritage platform from Airbus and an instr
ument by ABB Canada. Both satellites will provide scientific data highly c
omplementary to existing and upcoming exoplanet related space and ground-b
ased observatories\, including NASA/ESA/CSA’s James Webb Space Telescope a
nd ESO’s Extremely Large Telescope.
\nBlue Skies Space is able to de
liver Mauve and Twinkle thanks to the substantial transformations currentl
y on-going in the space sector in Europe and beyond. Blue Skies Space Ital
ia S.R.L. was set up this year to leverage the capabilities and expertise
of the Italian science and technology community and help coordinate Europe
an science\, technology and funding activities.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24201@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221115T100000
DTEND;TZID=Europe/Rome:20221115T130000
SEQUENCE:0
SUMMARY:Visita Filippo Mirabello e ospiti
URL:http://www.astropa.inaf.it/evento/visita-filippo-mirabello-e-ospiti/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24203@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221116T110000
DTEND;TZID=Europe/Rome:20221116T130000
SEQUENCE:0
SUMMARY:Riunione con personale ASU
URL:http://www.astropa.inaf.it/evento/riunione-con-personale-asu/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24151@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Antonio Maggio
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221122T084500
DTEND;TZID=Europe/Rome:20221123T133000
SEQUENCE:0
SUMMARY:Concorso INAF MA-2\, ARTICOLAZIONE 2.3 “INTERAZIONE STELLA – PIANET
A” – Posizione 10
URL:http://www.astropa.inaf.it/evento/concorso-inaf-ma-2-articolazione-2-3-
interazione-stella-pianeta-posizione-10/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
X-TAGS;LANGUAGE=it-IT:Prova orale concorso
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24155@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:Antonio Maggio
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221123T143000
DTEND;TZID=Europe/Rome:20221125T144500
SEQUENCE:0
SUMMARY:Meeting THE StellaR PAth
URL:http://www.astropa.inaf.it/evento/meeting-the-stellar-path-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
X-TAGS;LANGUAGE=it-IT:exoplanets
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24234@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Stanza Google Meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Gloria Guilluy (INAF-OATo)\nTitolo: Exoplanetary Atmospheres with GIAN
O@TNG.\nAbstract: I will present the atmospheric characterization study of
hot and warm giant planets using the Telescopio Nazionale Galileo (TNG) i
n the simultaneous GIARPS (GIANO-B + HARPS-N) observing mode. I will focus
in particular on our ongoing efforts to probe both the lower and the uppe
r exoplanetary atmospheres using the near-infrared (0.95-2.45 \\mu m) arm
of GIARPS: the high-resolution (R /sim 50 000) spectrograph GIANO-B. On th
e one hand\, I will discuss our investigations of the deeper exo-atmospher
ic layers performed through the search of molecular species (e.g.\, water\
, methane\, carbon dioxide\, hydrogen cyanide) which\, by constraining the
planet’s C/O ratio\, provide clear proxies on planetary formation. On the
other hand\, I will show our upper exoplanetary atmospheres’ analysis rea
lized through the detection of the individual contributions of atoms (more
precisely the metastable helium line at 1083.3 nm). The helium line\, in
addition to providing key insights into an exoplanetary exosphere\, allows
for putting constraints on evolutionary processes (i.e. hydrodynamic esca
pe\, the mass loss rate\, and the morphology of the escaping material).
DTSTART;TZID=Europe/Rome:20221125T110000
DTEND;TZID=Europe/Rome:20221125T123000
SEQUENCE:0
SUMMARY:Seminario: Gloria Guilluy (INAF-OATo)
URL:http://www.astropa.inaf.it/evento/seminario-gloria-guilluy-inaf-oato/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n\n
Stanza Google Meet:
https://meet.google.com/sxz-cctp-tsc
\n
Speaker: Gloria Guilluy (INAF-OATo)
\n
Titolo: Exoplanetary Atmospheres with GIANO@TNG.
\n
Abstract: I will present the atmospheric characterizati
on study of hot and warm giant planets using the Telescopio Nazionale Gali
leo (TNG) in the simultaneous GIARPS (GIANO-B + HARPS-N) observing mode. I
will focus in particular on our ongoing efforts to probe both the lower a
nd the upper exoplanetary atmospheres using the near-infrared (0.95-2.45 \
\mu m) arm of GIARPS: the high-resolution (R /sim 50 000) spectrograph GIA
NO-B. On the one hand\, I will discuss our investigations of the deeper ex
o-atmospheric layers performed through the search of molecular species (e.
g.\, water\, methane\, carbon dioxide\, hydrogen cyanide) which\, by const
raining the planet’s C/O ratio\, provide clear proxies on planetary format
ion. On the other hand\, I will show our upper exoplanetary atmospheres’ a
nalysis realized through the detection of the individual contributions of
atoms (more precisely the metastable helium line at 1083.3 nm). The helium
line\, in addition to providing key insights into an exoplanetary exosphe
re\, allows for putting constraints on evolutionary processes (i.e. hydrod
ynamic escape\, the mass loss rate\, and the morphology of the escaping ma
terial).
\n
\n\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24312@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221129T093000
DTEND;TZID=Europe/Rome:20221129T133000
SEQUENCE:0
SUMMARY:EXOPA
URL:http://www.astropa.inaf.it/evento/exopa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24267@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Concorso\,Aula: Esami
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221130T090000
DTEND;TZID=Europe/Rome:20221130T140000
SEQUENCE:0
SUMMARY:prova orale concorso tecnologi pos.4
URL:http://www.astropa.inaf.it/evento/prova-orale-concorso-tecnologi-pos-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24498@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:Discussione su polarizzazione e variabilita’ temporale dell’emi
ssione di sincrotrone in Kepler
DTSTART;TZID=Europe/Rome:20221212T110000
DTEND;TZID=Europe/Rome:20221212T131500
SEQUENCE:0
SUMMARY:Riunione gruppo SNR
URL:http://www.astropa.inaf.it/evento/riunione-gruppo-snr-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nDiscussione su polarizzazione e variabilita’ tempor
ale dell’emissione di sincrotrone in Kepler
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24497@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:Idee per proposte per il ciclo 2 di JWST e finalizzate allo stu
dio di esopianeti.
DTSTART;TZID=Europe/Rome:20221212T143000
DTEND;TZID=Europe/Rome:20221212T163000
SEQUENCE:0
SUMMARY:Riunione gruppo esopianeti (EXOPA)
URL:http://www.astropa.inaf.it/evento/riunione-gruppo-esopianeti-exopa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nIdee per proposte per il ciclo 2 di JWST e finalizz
ate allo studio di esopianeti.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24307@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Stanza Google Meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Ciro Pinto (INAF / IASF-Palermo)\nTitolo: “Fast growth and feedback of
black holes accreting beyond the Eddington limit”\nAbstract:\nThe detecti
on of fully-grown supermassive black holes in active galactic nuclei at hi
gh redshift\, when the Universe was young\, challenges the theories of bla
ck holes growth\, requiring long periods of high accretion\, most likely a
bove the Eddington limit. These objects will be difficult to study in deta
il\, even with future advanced observatories. In the nearby Universe there
are compact objects with a similar accretion regime that can be used as p
roxy for primordial black holes. Ultraluminous X-ray sources (ULXs) are ma
inly nearby stellar-mass black holes and neutron stars accreting above the
ir Eddington limit. This was understood after the discovery of coherent pu
lsations and cyclotron lines in some ULXs\, indicating that at least a fra
ction of them hosts neutron stars as compact objects and\, finally\, our d
iscovery of powerful winds as predicted by theoretical models of super-Edd
ington accretion. ULX winds carry a huge amount of power owing to their mi
ldly relativistic speeds (~0.2c) and are able to significantly affect the
surrounding medium\, producing the observed 100s pc super bubbles\, and li
mit the amount of matter that can reach the central accretor. The study of
ULX winds is therefore quintessential to understand 1) how much and how f
ast can matter be accreted by black holes and 2) how strong is their feedb
ack onto the surrounding medium in the regime of high accretion rate such
as for quasars and supermassive black holes at their peak of growth. I wil
l provide an overview on this phenomenology and discuss how we can use sim
ilar techniques onto highly-accreting supermassive black holes to understa
nd their fast growth and feedback onto the host galaxy.
DTSTART;TZID=Europe/Rome:20221215T150000
DTEND;TZID=Europe/Rome:20221215T163000
SEQUENCE:0
SUMMARY:Seminario: Ciro Pinto (INAF / IASF-Palermo)
URL:http://www.astropa.inaf.it/evento/seminario-ciro-pinto-inaf-iasf-palerm
o/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nStanza Google Meet: https://meet.google.com/sxz-cct
p-tsc
\nSpeaker: Ciro Pinto (INAF / IASF-Palermo)
\nTitolo: “F
ast growth and feedback of black holes accreting beyond the Eddington limi
t”
\nAbstract:
\nThe detection of fully-grown supermassive blac
k holes in active galactic nuclei at high redshift\, when the Universe was
young\, challenges the theories of black holes growth\, requiring long pe
riods of high accretion\, most likely above the Eddington limit. These obj
ects will be difficult to study in detail\, even with future advanced obse
rvatories. In the nearby Universe there are compact objects with a similar
accretion regime that can be used as proxy for primordial black holes. Ul
traluminous X-ray sources (ULXs) are mainly nearby stellar-mass black hole
s and neutron stars accreting above their Eddington limit. This was unders
tood after the discovery of coherent pulsations and cyclotron lines in som
e ULXs\, indicating that at least a fraction of them hosts neutron stars a
s compact objects and\, finally\, our discovery of powerful winds as predi
cted by theoretical models of super-Eddington accretion. ULX winds carry a
huge amount of power owing to their mildly relativistic speeds (~0.2c) an
d are able to significantly affect the surrounding medium\, producing the
observed 100s pc super bubbles\, and limit the amount of matter that can r
each the central accretor. The study of ULX winds is therefore quintessent
ial to understand 1) how much and how fast can matter be accreted by black
holes and 2) how strong is their feedback onto the surrounding medium in
the regime of high accretion rate such as for quasars and supermassive bla
ck holes at their peak of growth. I will provide an overview on this pheno
menology and discuss how we can use similar techniques onto highly-accreti
ng supermassive black holes to understand their fast growth and feedback o
nto the host galaxy.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24503@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Google meet: https://meet.google.com/sxz-cctp-tsc\nSpeaker: Ang
elo Adamo (INAF)\nTitolo: Domicili cosmici – Lontani pianeti ai confini de
llo sguardo\nAbstract: Si fa presto a dire “pianeta”\, un termine che semb
ra non richiedere mai precisazioni\, tanto appare ovvio\; banale\, quasi.
Eppure richiama alla mente un’immagine il cui significato (fra diaspore sp
aziali\, fughe e traslochi dal sapore fantascientifico capaci di modificar
e il senso e il valore di un concetto tanto semplice e comune quanto vago)
è cambiato più e più volte nel corso della storia\, dalle origini ai gior
ni nostri. In “Domicili cosmici” l’astrofisico\, divulgatore\, fumettista
e musicista Angelo Adamo raccoglie e organizza una grande quantità di idee
mutuate non solo dalla geologia\, dall’astronomia e dalla sua storia\, ma
anche dalla letteratura\, dalla poesia e dal cinema\, per ripercorrere le
tappe di questa continua trasformazione. E lo fa arricchendo il testo con
le sue tavole originali e suggestive\, veri e propri calembour disegnati\
, che si intrecciano con i giochi di parole e le espressioni matematiche d
isseminate nel testo. Il risultato è quasi un’antologia\, un compendio ill
ustrato di filosofia astronomica che racconta un’evoluzione culturale fatt
a di idee\, ipotesi\, suggestioni\, storie\, esperimenti\, simulazioni. E
speranze.
DTSTART;TZID=Europe/Rome:20221216T093000
DTEND;TZID=Europe/Rome:20221216T110000
SEQUENCE:0
SUMMARY:Seminario: presentazione del libro “Domicili Cosmici” di Angelo Ada
mo (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-angelo-adamo-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nGoogle meet: https://meet.google.com/sxz-cctp-tsc
p>\n
Speaker: Angelo Adamo (INAF)
\nTitolo: Domicili cosmici – Lon
tani pianeti ai confini dello sguardo
\nAbstract: Si fa presto a dir
e “pianeta”\, un termine che sembra non richiedere mai precisazioni\, tant
o appare ovvio\; banale\, quasi. Eppure richiama alla mente un’immagine il
cui significato (fra diaspore spaziali\, fughe e traslochi dal sapore fan
tascientifico capaci di modificare il senso e il valore di un concetto tan
to semplice e comune quanto vago) è cambiato più e più volte nel corso del
la storia\, dalle origini ai giorni nostri. In “Domicili cosmici” l’astrof
isico\, divulgatore\, fumettista e musicista Angelo Adamo raccoglie e orga
nizza una grande quantità di idee mutuate non solo dalla geologia\, dall’a
stronomia e dalla sua storia\, ma anche dalla letteratura\, dalla poesia e
dal cinema\, per ripercorrere le tappe di questa continua trasformazione.
E lo fa arricchendo il testo con le sue tavole originali e suggestive\, v
eri e propri calembour disegnati\, che si intrecciano con i giochi di paro
le e le espressioni matematiche disseminate nel testo. Il risultato è quas
i un’antologia\, un compendio illustrato di filosofia astronomica che racc
onta un’evoluzione culturale fatta di idee\, ipotesi\, suggestioni\, stori
e\, esperimenti\, simulazioni. E speranze.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24506@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20221219T110000
DTEND;TZID=Europe/Rome:20221219T133000
SEQUENCE:0
SUMMARY:Riunione Symposium SIC2023
URL:http://www.astropa.inaf.it/evento/riunione-symposium-sic2023/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24460@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230110T094500
DTEND;TZID=Europe/Rome:20230110T120000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24535@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Fabio Favata (ESA)\nTitolo: Agenzie spaziali e telesco
pi spaziali: un passato di grande successo\, un futuro incerto\nAbstract:
Il primo telescopio spaziale è stato lanciato nel 1968\, e per i ricercato
ri del XXI secolo l’esistenza di una flotta di telescopi in orbita\, acces
sibile a qualsiasi ricercatore qualificato\, è data per acquisita. È anche
spesso dato per scontato che ciascuna generazione di telescopi spaziali s
ia seguita da una generazione di telescopi più potenti. Le agenzie spazial
i nazionali (come la NASA negli USA\, o l’ASI in Italia) e quelle internaz
ionali (come l’ESA in Europa) sono spesso percepite come lo strumento isti
tuzionale al servizio della comunità scientifica\, a cui è affidato il ruo
lo di tradurre in realtà i progetti scientifici dei ricercatori. Questa pe
rcezione è stata abbastanza fedele alla realtà nei 50 anni trascorsi dal l
ancio del primo telescopio spaziale.\nNel frattempo però l’ecosistema spaz
iale mondiale è cambiato enormemente\, così come sono cambiate le dinamich
e e la governance delle agenzie spaziali\, e oggi è tutt’altro che evident
e che l’approccio che ha portato a enormi successi nei 50 passati possa co
ntinuare a funzionare in futuro. In parole povere\, non è affatto scontato
che il modello che ha portato a questi successi sia adeguato ad affrontar
e le sfide odierne.\nChi lavora nelle agenzie spesso nota che la comunità
scientifica non è necessariamente al corrente di come un’agenzia funziona\
, di quali sono le dinamiche attraverso cui vengono prese le decisioni chi
ave che determinano il futuro della scienza spaziale. Di conseguenza spess
o non è chiaro ai ricercatori come agire in maniera efficace per far sì ch
e la scienza dallo spazio continui in futuro ad avere successo.\nIl semina
rio intende fornire una visione di come funziona un’Agenzia Spaziale (in p
articolare l’ESA) e di quali sono le sfide epocali a cui va incontro oggi
la scienza spaziale.
DTSTART;TZID=Europe/Rome:20230111T150000
DTEND;TZID=Europe/Rome:20230111T170000
SEQUENCE:0
SUMMARY:Seminario: Fabio Favata (ESA)
URL:http://www.astropa.inaf.it/evento/seminario-fabio-favata-esa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Fabio Favata (ESA)
\nTitolo: Agenzie
spaziali e telescopi spaziali: un passato di grande successo\, un futuro
incerto
\nAbstract: Il primo telescopio spaziale è stato lanciato ne
l 1968\, e per i ricercatori del XXI secolo l’esistenza di una flotta di t
elescopi in orbita\, accessibile a qualsiasi ricercatore qualificato\, è d
ata per acquisita. È anche spesso dato per scontato che ciascuna generazio
ne di telescopi spaziali sia seguita da una generazione di telescopi più p
otenti. Le agenzie spaziali nazionali (come la NASA negli USA\, o l’ASI in
Italia) e quelle internazionali (come l’ESA in Europa) sono spesso percep
ite come lo strumento istituzionale al servizio della comunità scientifica
\, a cui è affidato il ruolo di tradurre in realtà i progetti scientifici
dei ricercatori. Questa percezione è stata abbastanza fedele alla realtà n
ei 50 anni trascorsi dal lancio del primo telescopio spaziale.
\nNel
frattempo però l’ecosistema spaziale mondiale è cambiato enormemente\, cos
ì come sono cambiate le dinamiche e la governance delle agenzie spaziali\,
e oggi è tutt’altro che evidente che l’approccio che ha portato a enormi
successi nei 50 passati possa continuare a funzionare in futuro. In parole
povere\, non è affatto scontato che il modello che ha portato a questi su
ccessi sia adeguato ad affrontare le sfide odierne.
\nChi lavora nell
e agenzie spesso nota che la comunità scientifica non è necessariamente al
corrente di come un’agenzia funziona\, di quali sono le dinamiche attrave
rso cui vengono prese le decisioni chiave che determinano il futuro della
scienza spaziale. Di conseguenza spesso non è chiaro ai ricercatori come a
gire in maniera efficace per far sì che la scienza dallo spazio continui i
n futuro ad avere successo.
\nIl seminario intende fornire una vision
e di come funziona un’Agenzia Spaziale (in particolare l’ESA) e di quali s
ono le sfide epocali a cui va incontro oggi la scienza spaziale.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24647@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230112T120000
DTEND;TZID=Europe/Rome:20230112T130000
SEQUENCE:0
SUMMARY:Riunione del Direttore su Museo
URL:http://www.astropa.inaf.it/evento/riunione-del-direttore-su-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24517@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Stanza Google Meet: https://meet.google.com/sxz-cctp-tsc\nSpeak
er: Darius Modirrousta-Galian (Yale University)\nTitle: The three regimes
of atmospheric evaporation for super-Earths and sub-Neptunes\nAbstract:\nA
significant fraction of super-Earths and sub-Neptunes are thought to expe
rience an extreme loss of volatiles because of atmospheric evaporation in
the early stages of their life. Though the mechanisms behind the extreme m
ass loss are not fully understood\, two contenders have been widely discus
sed: photoevaporation from X-ray and ultraviolet irradiation and core powe
red mass loss. In this talk\, I will discuss the new model of Modirrousta-
Galian & Korenaga\, suggesting that both mechanisms occur but with differe
nt timescales and that atmospheric evaporation can be classified under thr
ee regimes. This talk will summarize by explaining why the next step in ex
oplanetary science is to incorporate more realistic formational and geophy
sical modeling\, and how such models could be tested through observations.
DTSTART;TZID=Europe/Rome:20230112T150000
DTEND;TZID=Europe/Rome:20230112T170000
SEQUENCE:0
SUMMARY:Seminario online: Darius Modirrousta-Galian (Yale University)
URL:http://www.astropa.inaf.it/evento/seminario-online-darius-modirrousta-g
alian-yale-university/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nStanza Google Meet: https://meet.google.com/sxz-cct
p-tsc
\nSpeaker: Darius Modirrousta-Galian (Yale University)
\nTitle: The three regimes of atmospheric evaporation for super-Earths and
sub-Neptunes
\nAbstract:
\nA significant fraction of super-Ear
ths and sub-Neptunes are thought to experience an extreme loss of volatile
s because of atmospheric evaporation in the early stages of their life. Th
ough the mechanisms behind the extreme mass loss are not fully understood\
, two contenders have been widely discussed: photoevaporation from X-ray a
nd ultraviolet irradiation and core powered mass loss. In this talk\, I wi
ll discuss the new model of Modirrousta-Galian & Korenaga\, suggesting tha
t both mechanisms occur but with different timescales and that atmospheric
evaporation can be classified under three regimes. This talk will summari
ze by explaining why the next step in exoplanetary science is to incorpora
te more realistic formational and geophysical modeling\, and how such mode
ls could be tested through observations.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24648@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230117T110000
DTEND;TZID=Europe/Rome:20230117T120000
SEQUENCE:0
SUMMARY:Riunione Direttore Calcolo PNRR
URL:http://www.astropa.inaf.it/evento/riunione-direttore-calcolo-pnrr/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24649@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230118T110000
DTEND;TZID=Europe/Rome:20230118T130000
SEQUENCE:0
SUMMARY:Riunione Ufficio Acquisti
URL:http://www.astropa.inaf.it/evento/riunione-ufficio-acquisti/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24459@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230124T094500
DTEND;TZID=Europe/Rome:20230124T120000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-23859@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:Riunione di gruppo SNR
DTSTART;TZID=Europe/Rome:20230125T110000
DTEND;TZID=Europe/Rome:20230125T130000
SEQUENCE:0
SUMMARY:Riunione SNR
URL:http://www.astropa.inaf.it/evento/riunione-snr-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRiunione di gruppo SNR
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24646@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:60 pax
DTSTART;TZID=Europe/Rome:20230127T083000
DTEND;TZID=Europe/Rome:20230127T130000
SEQUENCE:0
SUMMARY:Visita S. Anna
URL:http://www.astropa.inaf.it/evento/visita-s-anna/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n60 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25009@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230210T090000
DTEND;TZID=Europe/Rome:20230210T130000
SEQUENCE:0
SUMMARY:Visita scolaresca Liceo G. Galilei
URL:http://www.astropa.inaf.it/evento/visita-scolaresca-liceo-g-galilei/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24461@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230214T094500
DTEND;TZID=Europe/Rome:20230214T120000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25102@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230215T083000
DTEND;TZID=Europe/Rome:20230215T130000
SEQUENCE:0
SUMMARY:Colleghi INAF
URL:http://www.astropa.inaf.it/evento/colleghi-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25126@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Ref (Inzerillo – Coniglio)
DTSTART;TZID=Europe/Rome:20230220T103000
DTEND;TZID=Europe/Rome:20230220T130000
SEQUENCE:0
SUMMARY:Visita Museo ore 11
URL:http://www.astropa.inaf.it/evento/visita-museo-ore-11/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRef (Inzerillo – Coniglio)
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25210@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230221T100000
DTEND;TZID=Europe/Rome:20230221T120000
SEQUENCE:0
SUMMARY:Riunione progetto CRA
URL:http://www.astropa.inaf.it/evento/riunione-progetto-cra/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-24462@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230228T094500
DTEND;TZID=Europe/Rome:20230228T120000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25249@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230302T143000
DTEND;TZID=Europe/Rome:20230302T160000
SEQUENCE:0
SUMMARY:visita museo – 3 pax VIsalli
URL:http://www.astropa.inaf.it/evento/visita-museo-3-pax-visalli/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25274@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Google meet: https://meet.google.com/sxz-cctp-tsc\nSpeaker: Gia
nluca Cracchiolo (UNIPA)\nTitle: Mitigation of the impact of stellar activ
ity on observations of transiting planets\nAbstract: In the thesis I devol
op different methods to correct the planetary transmission spectra for the
effect of unocculted stellar spots. The methods are based on stellar acti
vity models of increasing complexity\, from models of spotted stars assumi
ng a uniform stellar emission to models including the limb darkening effec
t. The correction strategies are developed for low-resolution observations
from space and applied to simulations of observations with Ariel\, the fu
ture space mission devoted to the observation of about 1000 exoatmospheres
. These techniques are applied to the transit observation of the Super-Ear
th LHS 1140 b of December 2017\, acquired with the WFC3/HST. The analysis
shows that the out-of transit stellar spectrum can be fitted with a model
of active star with a photospheric temperature of 3219 K and a spot distri
bution 400 K cooler and covering a fraction of 45-60% of the stellar disk\
, or with a model of quiet but cooler star (2916 K). In both cases\, the d
erived planet’s transmission spectra are flat spectra\, without any eviden
ce of molecular absorption bands. A similar approach is used to model the
TESS observations of V1298 Tau\, a pre-mai sequence star hosting 4 exoplan
ets. I show that the stellar variability of V1298 Tau can be fitted with a
4-spot model\, not evolving and rotating with the stellar surface. I corr
ect the transit light curves of the 4 planets for the presence of spots (a
ssumed to be not-crossed) and I estimate the effect that the same spots wo
uld cause on simultaneous observations in the K2 band. The results show th
at the effect is dependent on both the observation band and the spots’ con
figuration at the time of the transit.
DTSTART;TZID=Europe/Rome:20230306T153000
DTEND;TZID=Europe/Rome:20230306T170000
SEQUENCE:0
SUMMARY:Seminario: presentazione tesi dottorato di G. Cracchiolo (UNIPA)\,
Aula ore 15
URL:http://www.astropa.inaf.it/evento/seminario-presentazione-tesi-dottorat
o-di-g-cracchiolo-unipa-aula-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nGoogle meet: https://meet.google.com/sxz-cctp-tsc
p>\n
Speaker: Gianluca Cracchiolo (UNIPA)
\nTitle: Mitigation of t
he impact of stellar activity on observations of transiting planets
\n<
p>Abstract: In the thesis I devolop different methods to correct the plane
tary transmission spectra for the effect of unocculted stellar spots. The
methods are based on stellar activity models of increasing complexity\, fr
om models of spotted stars assuming a uniform stellar emission to models i
ncluding the limb darkening effect. The correction strategies are develope
d for low-resolution observations from space and applied to simulations of
observations with Ariel\, the future space mission devoted to the observa
tion of about 1000 exoatmospheres. These techniques are applied to the tra
nsit observation of the Super-Earth LHS 1140 b of December 2017\, acquired
with the WFC3/HST. The analysis shows that the out-of transit stellar spe
ctrum can be fitted with a model of active star with a photospheric temper
ature of 3219 K and a spot distribution 400 K cooler and covering a fracti
on of 45-60% of the stellar disk\, or with a model of quiet but cooler sta
r (2916 K). In both cases\, the derived planet’s transmission spectra are
flat spectra\, without any evidence of molecular absorption bands. A simil
ar approach is used to model the TESS observations of V1298 Tau\, a pre-ma
i sequence star hosting 4 exoplanets. I show that the stellar variability
of V1298 Tau can be fitted with a 4-spot model\, not evolving and rotating
with the stellar surface. I correct the transit light curves of the 4 pla
nets for the presence of spots (assumed to be not-crossed) and I estimate
the effect that the same spots would cause on simultaneous observations in
the K2 band. The results show that the effect is dependent on both the ob
servation band and the spots’ configuration at the time of the transit.\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25275@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speakers: Caterina Boccato\, Marco Galliani\, Marco Malaspina (
INAF)\nTitolo: Comunicazione@INAF\nAbstract: La terza missione sta diventa
ndo sempre più cruciale per enti di ricerca e atenei\, in particolare tutt
e quelle attività che vanno sotto il nome di Public Engagement o\, se pref
erite\, Comunicazione nel senso più ampio del termine. Attività che vedono
coinvolti\, in prima persona\, sempre più ricercatori e ricercatrici.\nIn
questo incontro vorremmo fornirvi alcuni strumenti per orientarvi al megl
io e per collaborare secondo le attitudini e le aspirazioni di ciascuno di
voi\, ma anche dirvi com’è articolata la Struttura per la comunicazione d
ell’INAF.\nMa\, soprattutto\, vorremmo dare risposta alle tante domande ch
e spesso ci ponete: cosa si intende per press release\, news\, conferenza
stampa\, embargo\, comunicato congiunto\, virgolettato e cose simili? A ch
i vi rivolgete? Cosa posso raccontare a bambini e bambine di sei anni? Per
ché a volte avete così fretta di contattarmi mentre sono impegnato in un m
eeting o una call? Perché non mi hanno accettato al festival della scienza
? E\, soprattutto\, perché parlate di qualunque cosa tranne che delle mie
ricerche?\n
DTSTART;TZID=Europe/Rome:20230310T113000
DTEND;TZID=Europe/Rome:20230310T130000
SEQUENCE:0
SUMMARY:Seminario: Comunicazione@INAF C. Boccato\, M. Galliani\, M. Malaspi
na (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-comunicazioneinaf-c-boccato
-m-galliani-m-malaspina-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeakers: Caterina Boccato\, Marco Galliani\, Marco
Malaspina (INAF)
\nTitolo: Comunicazione@INAF
\nAbstract: La
terza missione sta diventando sempre più cruciale per enti di ricerca e at
enei\, in particolare tutte quelle attività che vanno sotto il nome di Pub
lic Engagement o\, se preferite\, Comunicazione nel senso più ampio del te
rmine. Attività che vedono coinvolti\, in prima persona\, sempre più ricer
catori e ricercatrici.
\nIn questo incontro vorremmo fornirvi alcuni
strumenti per orientarvi al meglio e per collaborare secondo le attitudin
i e le aspirazioni di ciascuno di voi\, ma anche dirvi com’è articolata la
Struttura per la comunicazione dell’INAF.
\nMa\, soprattutto\, vorr
emmo dare risposta alle tante domande che spesso ci ponete: cosa si intend
e per press release\, news\, conferenza stampa\, embargo\, comunicato cong
iunto\, virgolettato e cose simili? A chi vi rivolgete? Cosa posso raccont
are a bambini e bambine di sei anni? Perché a volte avete così fretta di c
ontattarmi mentre sono impegnato in un meeting o una call? Perché non mi h
anno accettato al festival della scienza? E\, soprattutto\, perché parlate
di qualunque cosa tranne che delle mie ricerche?
\n
\n
HTML>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25654@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230314T094500
DTEND;TZID=Europe/Rome:20230314T120000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-4-2-2-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25327@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Sara Bonito
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230316T093000
DTEND;TZID=Europe/Rome:20230316T110000
SEQUENCE:0
SUMMARY:Riunione gruppo Realta’ Virtuale OAPa
URL:http://www.astropa.inaf.it/evento/riunione-gruppo-realta-virtuale-oapa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25304@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:ref. Chinnici\n1 o 2 turni di visita
DTSTART;TZID=Europe/Rome:20230317T150000
DTEND;TZID=Europe/Rome:20230317T180000
SEQUENCE:0
SUMMARY:Visite museo Convitto Nazionale
URL:http://www.astropa.inaf.it/evento/visite-museo-convitto-nazionale/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nref. Chinnici
\n1 o 2 turni di visita
\n
BODY>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25356@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:rif. Chinnci
DTSTART;TZID=Europe/Rome:20230317T160000
DTEND;TZID=Europe/Rome:20230317T191500
SEQUENCE:0
SUMMARY:visite museo convitto nazionale
URL:http://www.astropa.inaf.it/evento/visite-museo-convitto-nazionale-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nrif. Chinnci
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25128@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:Visite al Museo\, Presentazioni in aula\, Osservazioni del sole
(ref Daricello)
DTSTART;TZID=Europe/Rome:20230320T080000
DTEND;TZID=Europe/Rome:20230320T140000
RDATE;TZID=Europe/Rome:20230321T080000
RDATE;TZID=Europe/Rome:20230322T080000
RDATE;TZID=Europe/Rome:20230323T080000
RDATE;TZID=Europe/Rome:20230324T080000
SEQUENCE:0
SUMMARY:Light in Astronomy
URL:http://www.astropa.inaf.it/evento/light-in-astronomy/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nVisite al Museo\, Presentazioni in aula\, Osservazi
oni del sole (ref Daricello)
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25354@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Rif Chinnici
DTSTART;TZID=Europe/Rome:20230321T163000
DTEND;TZID=Europe/Rome:20230321T183000
SEQUENCE:0
SUMMARY:Visita al Museo 1 Pax (Chinnici)
URL:http://www.astropa.inaf.it/evento/visita-al-museo-1-pax-chinnici/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRif Chinnici
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25355@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:osservazione della prima falce di Luna per l’inizio del mese di
Ramadam del calendario islamico (rif. Direttore)
DTSTART;TZID=Europe/Rome:20230322T161500
DTEND;TZID=Europe/Rome:20230322T200000
SEQUENCE:0
SUMMARY:Visita delegazione di Imam in OAPa (rif. Direttore)
URL:http://www.astropa.inaf.it/evento/visita-delegazione-di-imam-in-oapa-ri
f-direttore/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nosservazione della prima falce di Luna per l’inizio
del mese di Ramadam del calendario islamico (rif. Direttore)
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25388@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230323T150000
DTEND;TZID=Europe/Rome:20230323T171500
SEQUENCE:0
SUMMARY:Riunione EXOPA terza missione
URL:http://www.astropa.inaf.it/evento/riunione-exopa-4-2-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25256@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230327T150000
DTEND;TZID=Europe/Rome:20230327T191500
SEQUENCE:0
SUMMARY:Visita e seminario per i bambini di Save The Children (Punto Luce Z
en)
URL:http://www.astropa.inaf.it/evento/visita-e-seminario-per-i-bambini-di-s
ave-the-children-punto-luce-zen/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25366@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Salvo Speziale\; salvatore.speziale@inaf.it
DESCRIPTION:Il set serve alla ripresa fotografica per la preparazione del m
odello 3D dello strumento e delle pertinenze.\n
DTSTART;TZID=Europe/Rome:20230329T090000
DTEND;TZID=Europe/Rome:20230407T100000
LOCATION:Museo
SEQUENCE:0
SUMMARY:Ripresa fotogrammetrica del Cerchio di Ramsden
URL:http://www.astropa.inaf.it/evento/ripresa-fotogrammetrica-del-cerchio-d
i-ramsden/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nIl set serve alla ripresa fotografica per la prepar
azione del modello 3D dello strumento e delle pertinenze.
\n
\n<
/BODY>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25452@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Aula: Teleconferenza
CONTACT:Sara Bonito\; rosaria.bonito@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230404T100000
DTEND;TZID=Europe/Rome:20230404T113000
SEQUENCE:0
SUMMARY:Riunione gruppo stellare
URL:http://www.astropa.inaf.it/evento/riunione-gruppo-stellare/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25524@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:rif. Guarcello
DTSTART;TZID=Europe/Rome:20230406T090000
DTEND;TZID=Europe/Rome:20230406T110000
SEQUENCE:0
SUMMARY:visita museo
URL:http://www.astropa.inaf.it/evento/visita-museo-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nrif. Guarcello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25523@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:rif. Daricello
DTSTART;TZID=Europe/Rome:20230411T110000
DTEND;TZID=Europe/Rome:20230411T130000
SEQUENCE:0
SUMMARY:Riunione servizio civile
URL:http://www.astropa.inaf.it/evento/riunione-servizio-civile/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nrif. Daricello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25130@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:Ref. Daricello
DTSTART;TZID=Europe/Rome:20230413T080000
DTEND;TZID=Europe/Rome:20230413T140000
SEQUENCE:0
SUMMARY:Visite Museo e Seminari e osservazioni sole Studenti Fisica Congres
so Nazionale
URL:http://www.astropa.inaf.it/evento/visite-museo-e-seminari-e-osservazion
i-sole-studenti-fisica-congresso-nazionale/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRef. Daricello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25450@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:rif. Daricello\n20 pax istituto Format
DTSTART;TZID=Europe/Rome:20230418T090000
DTEND;TZID=Europe/Rome:20230418T123000
SEQUENCE:0
SUMMARY:Visita museo e osservazioni del sole
URL:http://www.astropa.inaf.it/evento/visita-museo-e-osservazioni-del-sole/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nrif. Daricello
\n20 pax istituto Format
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25653@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230418T100000
DTEND;TZID=Europe/Rome:20230418T120000
SEQUENCE:0
SUMMARY:Riunione EXOPA terza missione
URL:http://www.astropa.inaf.it/evento/riunione-exopa-4-2-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25562@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:Rif. Benatti – Daricello
DTSTART;TZID=Europe/Rome:20230418T150000
DTEND;TZID=Europe/Rome:20230418T170000
SEQUENCE:0
SUMMARY:Riunione Ariel – comunicazione
URL:http://www.astropa.inaf.it/evento/riunione-ariel-comunicazione/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRif. Benatti – Daricello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25639@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:rif. Daricello\n20 pax
DTSTART;TZID=Europe/Rome:20230419T103000
DTEND;TZID=Europe/Rome:20230419T123000
SEQUENCE:0
SUMMARY:visita museo IISS Amato Vetrano Sciacca
URL:http://www.astropa.inaf.it/evento/visita-museo-scuola-sciacca/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nrif. Daricello
\n20 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25564@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Ricevimento studenti\,Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230427T090000
DTEND;TZID=Europe/Rome:20230427T110000
SEQUENCE:0
SUMMARY:visita Museo scolaresca
URL:http://www.astropa.inaf.it/evento/visita-museo-scolaresca/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25611@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:9\n10.30\nrif. Daricello
DTSTART;TZID=Europe/Rome:20230504T090000
DTEND;TZID=Europe/Rome:20230504T130000
SEQUENCE:0
SUMMARY:Visita museo istituto volta caltanissetta
URL:http://www.astropa.inaf.it/evento/visita-museo-istituto-volta-caltaniss
etta/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n9
\n10.30
\nrif. Daricello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25699@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:rif daricello\n2 turni 9 e 11\nVisita Museo I.C. Perez – Madre
Teresa di Calcutta
DTSTART;TZID=Europe/Rome:20230509T090000
DTEND;TZID=Europe/Rome:20230509T130000
SEQUENCE:0
SUMMARY:Visita Museo I.C. Perez – Madre Teresa di Calcutta 32 pax
URL:http://www.astropa.inaf.it/evento/visita-museo-i-c-perez-madre-teresa-d
i-calcutta-12-pax/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nrif daricello
\n2 turni 9 e 11
\nVisita Museo I.C. Perez – Madre Teresa di Calcut
ta
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25318@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230509T100000
DTEND;TZID=Europe/Rome:20230509T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-4-2-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25719@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Angelo Adamo (INAF)\nTitolo: Nati sotto il segno di Di
ke\, cresciuti con quello della Bilancia – La storia della Space Law\, tra
gravità e giurisprudenza\nAbstract:\nIn questo seminario pongo l’attenzio
ne su quei particolari momenti in cui la scienza giuridica ha felicemente
intersecato l’osservazione pre-scientifica della natura e\, in seguito\, l
e scienze fisiche propriamente dette\, traendo da esse\, specie nel passat
o\, quando ispirazione\, quando una maggiore forza argomentativa. Si tratt
a di incroci che sembrano denunciare in modo chiaro un’origine comune dell
o sguardo del fisico e del giurista – un’origine di sicuro meritevole di u
no studio storico e filosofico più attento che già sto conducendo – e che
la presente ricerca evidenzia solo per la parte avente a che fare con la d
escrizione di come la nostra specie si è progressivamente impossessata del
lo spazio esplorabile: un concetto usato in una fase iniziale esclusivamen
te per indicare territori sulla terraferma e che\, al progressivo crescere
delle acquisizioni scientifiche\, tecnologiche e di una parallela evoluzi
one giuridica\, ha subito diverse modifiche che gli hanno fatto guadagnare
pure il significato di distese marine\, di spazi aerei al di sopra delle
nazioni e\, in tempi più recenti\, quello di spazio esterno alla nostra at
mosfera. Uno spazio oramai teatro di dispute di diritto internazionale e s
cenario di possibili scontri bellici del futuro.
DTSTART;TZID=Europe/Rome:20230511T120000
DTEND;TZID=Europe/Rome:20230511T130000
SEQUENCE:0
SUMMARY:Seminario: Angelo Adamo (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-angelo-adamo-inaf-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Angelo Adamo (INAF)
\nTitolo: Nati so
tto il segno di Dike\, cresciuti con quello della Bilancia – La storia del
la Space Law\, tra gravità e giurisprudenza
\nAbstract:
\nIn qu
esto seminario pongo l’attenzione su quei particolari momenti in cui la sc
ienza giuridica ha felicemente intersecato l’osservazione pre-scientifica
della natura e\, in seguito\, le scienze fisiche propriamente dette\, trae
ndo da esse\, specie nel passato\, quando ispirazione\, quando una maggior
e forza argomentativa. Si tratta di incroci che sembrano denunciare in mod
o chiaro un’origine comune dello sguardo del fisico e del giurista – un’or
igine di sicuro meritevole di uno studio storico e filosofico più attento
che già sto conducendo – e che la presente ricerca evidenzia solo per la p
arte avente a che fare con la descrizione di come la nostra specie si è pr
ogressivamente impossessata dello spazio esplorabile: un concetto usato in
una fase iniziale esclusivamente per indicare territori sulla terraferma
e che\, al progressivo crescere delle acquisizioni scientifiche\, tecnolog
iche e di una parallela evoluzione giuridica\, ha subito diverse modifiche
che gli hanno fatto guadagnare pure il significato di distese marine\, di
spazi aerei al di sopra delle nazioni e\, in tempi più recenti\, quello d
i spazio esterno alla nostra atmosfera. Uno spazio oramai teatro di disput
e di diritto internazionale e scenario di possibili scontri bellici del fu
turo.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25703@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Serena Benatti\; serena.benatti@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230516T180000
DTEND;TZID=Europe/Rome:20230516T200000
SEQUENCE:0
SUMMARY:Visita Meeting Ariel-IT
URL:http://www.astropa.inaf.it/evento/visita-meeting-ariel-it/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25657@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:rif Daricello
DTSTART;TZID=Europe/Rome:20230524T090000
DTEND;TZID=Europe/Rome:20230524T130000
SEQUENCE:0
SUMMARY:museo +sole scuola piazzi
URL:http://www.astropa.inaf.it/evento/museo-sole-scuola-piazzi/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nrif Daricello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25727@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Flavio Morale\; flavio.morale@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230525T110000
DTEND;TZID=Europe/Rome:20230525T130000
LOCATION:Aula
SEQUENCE:0
SUMMARY:Visita Ufficio VIII\, Computing in Aula
URL:http://www.astropa.inaf.it/evento/visita-ufficio-viii-computing-in-aula
/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25310@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:8 ragazzi + 3 accompagnatori
DTSTART;TZID=Europe/Rome:20230605T100000
DTEND;TZID=Europe/Rome:20230605T130000
SEQUENCE:0
SUMMARY:Visita ragazzi Malaspina ref Daricello
URL:http://www.astropa.inaf.it/evento/visita-ragazzi-malaspina-ref-daricell
o/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n8 ragazzi + 3 accompagnatori
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25861@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:scuola piazzi 2 classi
DTSTART;TZID=Europe/Rome:20230606T090000
DTEND;TZID=Europe/Rome:20230606T130000
RDATE;TZID=Europe/Rome:20230607T090000
SEQUENCE:0
SUMMARY:visita museo piazzi
URL:http://www.astropa.inaf.it/evento/visita-museo-piazzi/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nscuola piazzi 2 classi
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25860@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:visita museo 2 pax
DTSTART;TZID=Europe/Rome:20230608T093000
DTEND;TZID=Europe/Rome:20230608T110000
SEQUENCE:0
SUMMARY:visita museo
URL:http://www.astropa.inaf.it/evento/visita-museo-5/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nvisita museo 2 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25767@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: M. G. Dainotti (National Astronomical Observatory of J
apan)\nTitle: The optical 2D and 3D correlation and their application as c
osmological tool\nAbstract: Gamma-ray bursts (GRBs) are fascinating events
due to their\npanchromatic nature. We study optical plateaus in GRB after
glows via\nan extended search into archival data. We comprehensively analy
ze all\npublished GRBs with known redshifts and optical plateaus observed
by\nmany ground-based telescopes (e.g.\, Subaru Telescope\, RATIR) around
\nthe world and several space-based observatories such as the Neil\nGehrel
s Swift Observatory. We fit 500 optical light curves\, showing\nthe existe
nce of the plateau in 179 cases. This sample is 75% larger\nthan the previ
ous one\, and it is the largest compilation so far of\noptical plateaus. W
e discover the 3D fundamental plane relation at\noptical wavelengths using
this sample. This correlation is between the\nrest-frame time at the end
of the plateau emission\, Topt * \, its\noptical luminosity\, Lopt\, and t
he peak in the optical prompt emission\,\nLpeak\,opt\, thus resembling the
three-dimensional (3D) X-ray\nfundamental plane (the so-called 3D Dainott
i relation). We correct our\nsample for redshift evolution and selection e
ffects\, discovering that\nthis correlation is indeed intrinsic to GRB phy
sics. We investigate\nthe rest-frame end-time distributions in X-rays and
optical (Topt * \,\nTX *)\, and conclude that the plateau is achromatic on
ly when selection\nbiases are not considered. We also investigate 3D optic
al correlation\nas a cosmological tool\, finding that it is as efficacious
as the X-ray\n3D correlation.
DTSTART;TZID=Europe/Rome:20230614T150000
DTEND;TZID=Europe/Rome:20230614T163000
SEQUENCE:0
SUMMARY:Seminario: Maria Giovanna Dainotti (NAOJ)
URL:http://www.astropa.inaf.it/evento/seminario-maria-giovanna-dainotti-nao
j/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: M. G. Dainotti (National Astronomical Obse
rvatory of Japan)
\nTitle: The optical 2D and 3D correlation and thei
r application as cosmological tool
\nAbstract: Gamma-ray bursts (GRB
s) are fascinating events due to their
\npanchromatic nature. We stud
y optical plateaus in GRB afterglows via
\nan extended search into ar
chival data. We comprehensively analyze all
\npublished GRBs with kno
wn redshifts and optical plateaus observed by
\nmany ground-based tel
escopes (e.g.\, Subaru Telescope\, RATIR) around
\nthe world and seve
ral space-based observatories such as the Neil
\nGehrels Swift Observ
atory. We fit 500 optical light curves\, showing
\nthe existence of t
he plateau in 179 cases. This sample is 75% larger
\nthan the previou
s one\, and it is the largest compilation so far of
\noptical plateau
s. We discover the 3D fundamental plane relation at
\noptical wavelen
gths using this sample. This correlation is between the
\nrest-frame
time at the end of the plateau emission\, Topt * \, its
\noptical lum
inosity\, Lopt\, and the peak in the optical prompt emission\,
\nLpea
k\,opt\, thus resembling the three-dimensional (3D) X-ray
\nfundament
al plane (the so-called 3D Dainotti relation). We correct our
\nsampl
e for redshift evolution and selection effects\, discovering that
\nt
his correlation is indeed intrinsic to GRB physics. We investigate
\n
the rest-frame end-time distributions in X-rays and optical (Topt * \,
\nTX *)\, and conclude that the plateau is achromatic only when selectio
n
\nbiases are not considered. We also investigate 3D optical correla
tion
\nas a cosmological tool\, finding that it is as efficacious as
the X-ray
\n3D correlation.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25560@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Museo
CONTACT:
DESCRIPTION:18 studenti della classe astrofisica e 15 studenti della classe
fisica\nviaggio virtuale nell’universo con realtà aumentata\nvisita guida
ta del museo della specola
DTSTART;TZID=Europe/Rome:20230615T090000
DTEND;TZID=Europe/Rome:20230615T130000
SEQUENCE:0
SUMMARY:Progetto Academy of Distinction (rif. Miceli – Daricello)
URL:http://www.astropa.inaf.it/evento/progetto-academy-of-distinction-rif-m
iceli-daricello/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n18 studenti della classe astrofisica e 15 studenti
della classe fisica
\nviaggio virtuale nell’universo con realtà aume
ntata
\nvisita guidata del museo della specola
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25970@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230620T100000
DTEND;TZID=Europe/Rome:20230620T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-5-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25967@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230620T110000
DTEND;TZID=Europe/Rome:20230620T130000
SEQUENCE:0
SUMMARY:Riunione sicurezza
URL:http://www.astropa.inaf.it/evento/riunione-sicurezza/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25971@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230622T100000
DTEND;TZID=Europe/Rome:20230622T130000
SEQUENCE:0
SUMMARY:Riunione RUP ed a seguire CdS
URL:http://www.astropa.inaf.it/evento/riunione-rup-ed-a-seguire-cds/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25952@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Claudia Di Maio\n\nTitle: The mass determination chall
enge for exoplanetary science\n\nAbstract:\n\nThe mass of an exoplanet is
a key parameter for the characterisation of the internal structure of a pl
anet\, as well as the study of the formation and the evolution of the plan
et\, and of its atmosphere.\nThe radial velocity technique allows measurin
g the planetary mass from the radial velocity variation of its parent star
. However\, limitations in the property determination of exoplanets\, part
icularly in their masses\, can arise from various sources especially from
astrophysical noise due to stellar variability\, caused by magnetic activi
ty\, which affects the detection and characterisation of exoplanets.\nDuri
ng my PhD\, I aim to understand the impact of our knowledge of the planeta
ry mass in the planetary atmospheric characterisation and to reduce the so
urces of uncertainty by a deep study of the stellar activity and by develo
ping new techniques\nfor stellar variability filtering.\n\n\nTo this end\,
I analysed the impact of the planetary mass uncertainties of atmospheric
retrievals of multiple targets from the mission reference sample of Ariel\
, the forthcoming ESA M4 mission aimed at studying planetary atmospheres.
\n\n\nI simulated different spectra as observed by Ariel\, assuming primor
dial or secondary atmospheres of hot Jupiters\, and sub-Neptunes or super-
Earths\, respectively\, under different cloudy configurations. I estimated
both the accuracy and precision necessary\nfor each analysed target\, tes
ting also the capability of retrieval in the case of incorrect mass estima
tion. I verified that one of the most crucial issues is the presence of hi
gh-altitude clouds\, in particular in the secondary atmosphere cases.\nFor
this reason\, I tested the capability to retrieve the cloudy configuratio
n or the presence of a secondary atmosphere during the first tier of the A
riel mission\, to take an informed decision if including the planet in the
Tier-2 sample.\n\nI also developed SpotCCF\, a photospheric stellar model
\, to optimise the radial velocity extraction in fast-rotating stars. This
model\, based on the cross-correlation function technique\, takes into ac
count the contribution of stellar activity by considering the presence of
multiple spots on the stellar surface that caused deformation of the profi
le of the cross-correlation function.\nGlobally\, I highlighted the import
ance of planetary mass characterization and the complexity of their determ
ination due to the effects of stellar variability. In the context of the A
riel mission\, it highlights the importance of a detailed and individual a
nalysis of each target of the mission reference sample\, to be able to acc
urately select the Tier-2 targets and characterise their planetary atmosph
ere\, and represents a step forward towards the preparation of the ESA M4
Ariel mission. It also shows how this work cannot be disentangled from a d
etailed study of the stellar variability that is crucial in the determinat
ion of the planetary mass\, both in its accuracy and precision.
DTSTART;TZID=Europe/Rome:20230622T150000
DTEND;TZID=Europe/Rome:20230622T163000
SEQUENCE:0
SUMMARY:Seminario: Claudia Di Maio (UNIPA/INAF)
URL:http://www.astropa.inaf.it/evento/seminario-claudia-di-maio-unipa-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Claudia Di Maio
\n\n
Title: Th
e mass determination challenge for exoplanetary science
\n
\n
Abstract:
\n
\n
The mass of an exoplanet is a key parame
ter for the characterisation of the internal structure of a planet\, as we
ll as the study of the formation and the evolution of the planet\, and of
its atmosphere.
\n
The radial velocity technique allows measuring t
he planetary mass from the radial velocity variation of its parent star. H
owever\, limitations in the property determination of exoplanets\, particu
larly in their masses\, can arise from various sources especially from ast
rophysical noise due to stellar variability\, caused by magnetic activity\
, which affects the detection and characterisation of exoplanets.
\n<
div>During my PhD\, I aim to understand the impact of our knowledge of the
planetary mass in the planetary atmospheric characterisation and to reduc
e the sources of uncertainty by a deep study of the stellar activity and b
y developing new techniques
\n
for stellar variability filtering.
\n
\n
\n
To this end\, I analysed the impact of the plan
etary mass uncertainties of atmospheric retrievals of multiple targets fro
m the mission reference sample of Ariel\, the forthcoming ESA M4 mission a
imed at studying planetary atmospheres.
\n
\n
\n
I simul
ated different spectra as observed by Ariel\, assuming primordial or secon
dary atmospheres of hot Jupiters\, and sub-Neptunes or super-Earths\, resp
ectively\, under different cloudy configurations. I estimated both the acc
uracy and precision necessary
\n
for each analysed target\, testi
ng also the capability of retrieval in the case of incorrect mass estimati
on. I verified that one of the most crucial issues is the presence of high
-altitude clouds\, in particular in the secondary atmosphere cases.
\n
For this reason\, I tested the capability to retrieve the cloudy co
nfiguration or the presence of a secondary atmosphere during the first tie
r of the Ariel mission\, to take an informed decision if including the pla
net in the Tier-2 sample.
\n
\n
I also developed SpotCCF\, a
photospheric stellar model\, to optimise the radial velocity extraction i
n fast-rotating stars. This model\, based on the cross-correlation functio
n technique\, takes into account the contribution of stellar activity by c
onsidering the presence of multiple spots on the stellar surface that caus
ed deformation of the profile of the cross-correlation function.
\n
Globally\, I highlighted the importance of planetary mass characterizat
ion and the complexity of their determination due to the effects of stella
r variability. In the context of the Ariel mission\, it highlights the imp
ortance of a detailed and individual analysis of each target of the missio
n reference sample\, to be able to accurately select the Tier-2 targets an
d characterise their planetary atmosphere\, and represents a step forward
towards the preparation of the ESA M4 Ariel mission. It also shows how thi
s work cannot be disentangled from a detailed study of the stellar variabi
lity that is crucial in the determination of the planetary mass\, both in
its accuracy and precision.\n
\n
\n\n\n
BODY>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25930@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Manuela Coniglio (INAF)\nTitolo: L’affresco dimenticat
o: celebrazione di una scoperta\nAbstract:\nL’Osservatorio Astronomico di
Palermo venne istituito alla fine del 1700\, in piena età neoclassica\, in
un momento storico in cui i cantieri borbonici realizzavano opere monumen
tali di grande interesse artistico e architettonico. A partire da tali pre
supposti\, sono stati condotti degli studi volti a rintracciare eventuali
elementi decorativi dell’originaria Specola panormitana\, oggi quasi del t
utto assenti. Il viaggio tra carte e documenti ha portato alla consultazio
ne di un variegato materiale archivistico\, composto da lettere e note man
oscritte ma anche disegni\, incisioni e fotografie\, conservati in diversi
archivi. Dal loro studio è emerso qualcosa di inaspettato e del tutto dim
enticato: un’imponente celebrazione artistica della scoperta di Cerere Fer
dinandea\, il primo asteroide individuato da Piazzi nella notte del 1° gen
naio 1801\, realizzata proprio nel Real Osservatorio di Palermo\, da cui i
l pianetino venne osservato per la prima volta.
DTSTART;TZID=Europe/Rome:20230628T150000
DTEND;TZID=Europe/Rome:20230628T163000
SEQUENCE:0
SUMMARY:Seminario: M. Coniglio (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-m-coniglio-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Manuela Coniglio (INAF)
\nTitolo: L’a
ffresco dimenticato: celebrazione di una scoperta
\nAbstract:
\n
L’Osservatorio Astronomico di Palermo venne istituito alla fine del 1700\,
in piena età neoclassica\, in un momento storico in cui i cantieri borbon
ici realizzavano opere monumentali di grande interesse artistico e archite
ttonico. A partire da tali presupposti\, sono stati condotti degli studi v
olti a rintracciare eventuali elementi decorativi dell’originaria Specola
panormitana\, oggi quasi del tutto assenti. Il viaggio tra carte e documen
ti ha portato alla consultazione di un variegato materiale archivistico\,
composto da lettere e note manoscritte ma anche disegni\, incisioni e foto
grafie\, conservati in diversi archivi. Dal loro studio è emerso qualcosa
di inaspettato e del tutto dimenticato: un’imponente celebrazione artistic
a della scoperta di Cerere Ferdinandea\, il primo asteroide individuato da
Piazzi nella notte del 1° gennaio 1801\, realizzata proprio nel Real Osse
rvatorio di Palermo\, da cui il pianetino venne osservato per la prima vol
ta.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25997@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230703T093000
DTEND;TZID=Europe/Rome:20230703T114500
SEQUENCE:0
SUMMARY:Visita museo 3 pax Giambelluca
URL:http://www.astropa.inaf.it/evento/visita-museo-3-pax-giambelluca/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26004@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Ref. Coniglio
DTSTART;TZID=Europe/Rome:20230704T090000
DTEND;TZID=Europe/Rome:20230704T130000
SEQUENCE:0
SUMMARY:
URL:http://www.astropa.inaf.it/evento/26004/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRef. Coniglio
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26011@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230704T100000
DTEND;TZID=Europe/Rome:20230704T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-5-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26006@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230705T110000
DTEND;TZID=Europe/Rome:20230705T130000
SEQUENCE:0
SUMMARY:Riunione Hyperteck S.r.L.
URL:http://www.astropa.inaf.it/evento/riunione-hyperteck-s-r-l/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26007@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230706T113000
DTEND;TZID=Europe/Rome:20230706T130000
SEQUENCE:0
SUMMARY:Riunione gestione documentale PNRR
URL:http://www.astropa.inaf.it/evento/riunione-gestione-documentale-pnrr/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25994@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230706T160000
DTEND;TZID=Europe/Rome:20230706T180000
SEQUENCE:0
SUMMARY:Riunione HPC (SCAN)
URL:http://www.astropa.inaf.it/evento/riunione-hpc-scan/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26001@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230710T110000
DTEND;TZID=Europe/Rome:20230710T130000
SEQUENCE:0
SUMMARY:Riunione RUP
URL:http://www.astropa.inaf.it/evento/riunione-rup-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26212@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230712T100000
DTEND;TZID=Europe/Rome:20230712T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-5-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26012@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230713T110000
DTEND;TZID=Europe/Rome:20230713T133000
SEQUENCE:0
SUMMARY:riunione rup
URL:http://www.astropa.inaf.it/evento/riunione-rup-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26097@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230907T100000
DTEND;TZID=Europe/Rome:20230907T130000
SEQUENCE:0
SUMMARY:exopa
URL:http://www.astropa.inaf.it/evento/exopa-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26196@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:F. Martines\; francesca.martines@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230912T090000
DTEND;TZID=Europe/Rome:20230912T153000
SEQUENCE:0
SUMMARY:Pulizia straordinaria Museo
URL:http://www.astropa.inaf.it/evento/pulizia-straordinaria-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26200@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230913T090000
DTEND;TZID=Europe/Rome:20230913T120000
SEQUENCE:0
SUMMARY:Prove per RAI cultura
URL:http://www.astropa.inaf.it/evento/prove-per-rai-cultura/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25972@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Formazione\,Museo
CONTACT:
DESCRIPTION:40 pax
DTSTART;TZID=Europe/Rome:20230918T170000
DTEND;TZID=Europe/Rome:20230918T210000
SEQUENCE:0
SUMMARY:Scuola di realtà virtuale Rif. Bonito
URL:http://www.astropa.inaf.it/evento/scuola-di-realta-virtuale-rif-bonito/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n40 pax
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26215@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230919T100000
DTEND;TZID=Europe/Rome:20230919T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-5-6/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25973@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230919T170000
DTEND;TZID=Europe/Rome:20230919T200000
RDATE;TZID=Europe/Rome:20230920T170000
RDATE;TZID=Europe/Rome:20230921T170000
RDATE;TZID=Europe/Rome:20230922T170000
SEQUENCE:0
SUMMARY:Congresso SIC visite al museo Rif. Chinnici
URL:http://www.astropa.inaf.it/evento/congresso-sic-visite-al-museo-rif-chi
nnici/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26211@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230920T110000
DTEND;TZID=Europe/Rome:20230920T130000
SEQUENCE:0
SUMMARY:Riunione Stelle M
URL:http://www.astropa.inaf.it/evento/riunione-stelle-m/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26219@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Mario Guarcello
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20230922T120000
DTEND;TZID=Europe/Rome:20230922T170000
SEQUENCE:0
SUMMARY:Riprese Rai Cultura
URL:http://www.astropa.inaf.it/evento/riprese-rai-cultura/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26186@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Google meet: https://meet.google.com/sxz-cctp-tsc\nSpeaker: Dr
David Pascoe (University of St Andrews)\nTitolo: Modern Diagnostic Techniq
ues for Stellar Atmospheres\nAbstract:\nThe high spatial and temporal reso
lution provided by the Solar Dynamics Observatory inspired the development
of advanced observational techniques to probe the solar atmosphere. For e
xample\, forward modelling of the EUV profile of coronal structures and th
e seismological analysis of magnetohydrodynamic waves provide powerful dia
gnostics to constrain properties such as the plasma density and magnetic f
ield strength. We also increasingly employ Bayesian analysis to increase t
he robustness and accuracy of our modelling. These techniques are now also
applied to study quasi-periodic pulsations associated with solar and stel
lar flares\, and our models are being extended to take advantage of in sit
u measurements from Solar Orbiter and Parker Solar Probe.
DTSTART;TZID=Europe/Rome:20230928T150000
DTEND;TZID=Europe/Rome:20230928T163000
SEQUENCE:0
SUMMARY:Seminario: David Pascoe (University of St Andrews)\, Aula ore 15
URL:http://www.astropa.inaf.it/evento/seminario-david-pascoe-university-of-
st-andrews-aula-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nGoogle meet: https://meet.google.com/sxz-cctp-tsc
p>\n
Speaker: Dr David Pascoe (University of St Andrews)
\nTitolo:
Modern Diagnostic Techniques for Stellar Atmospheres
\nAbstract:
\nThe high spatial and temporal resolution provided by the Solar Dynami
cs Observatory inspired the development of advanced observational techniqu
es to probe the solar atmosphere. For example\, forward modelling of the E
UV profile of coronal structures and the seismological analysis of magneto
hydrodynamic waves provide powerful diagnostics to constrain properties su
ch as the plasma density and magnetic field strength. We also increasingly
employ Bayesian analysis to increase the robustness and accuracy of our m
odelling. These techniques are now also applied to study quasi-periodic pu
lsations associated with solar and stellar flares\, and our models are bei
ng extended to take advantage of in situ measurements from Solar Orbiter a
nd Parker Solar Probe.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26228@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:GIUSEPPE SCOZZARO
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231002T090000
DTEND;TZID=Europe/Rome:20231002T110000
SEQUENCE:0
SUMMARY:riunione INAF_PNRR
URL:http://www.astropa.inaf.it/evento/riunione-inaf_pnrr/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26253@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231002T103000
DTEND;TZID=Europe/Rome:20231002T123000
SEQUENCE:0
SUMMARY:VideoConf con A. Fontana. Partecipano Direttore\, Salemi\, Scozzaro
\, Orlando
URL:http://www.astropa.inaf.it/evento/videoconf-con-a-fontana-partecipano-d
irettore-salemi-scozzaro-orlando/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26214@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231003T100000
DTEND;TZID=Europe/Rome:20231003T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-5-5/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26181@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Marco Tarantino Studente Magistrale in Statistica e Da
ta Science (LM-82)\, Universita’ degli Studi di Palermo\nTitolo:\nAPPLICA
ZIONE DI TECNICHE STATISTICHE PER LA PREVISIONE DELLA\nTEMPERATURA EFFETTI
VA DI STELLE GIOVANI\nAbstract:\nUno degli attuali argomenti di discussion
e riguarda la durata del processo di formazione di cluster stellari: vi so
no modelli teorici che ipotizzano un unico evento dal quale si formano tut
te le stelle appartenenti ad uno stesso cluster\, considerando un processo
di formazione rapido\, altri modelli che\, invece\, suppongono piu’ event
i di formazione\, tenendo conto di un processo di formazione lento. Uno de
i metodi piu’ utilizzati per ricavare l’eta’ delle stelle si basa sul conf
ronto della distribuzione delle stelle sul diagramma H-R con le isocrone t
eoriche. Una variabile fondamentale per applicare questo metodo e’ la tem
peratura efficace\, la quale si puo’ ricavare in maniera accurata dalla s
pettroscopia. Tuttavia\, nell’epoca delle grandi survey fotometriche\, e’
necessario derivare la temperatura efficace basandosi sulla fotometria. L’
obiettivo del lavoro consiste nel trovare un modello che permetta di otten
ere buone previsioni della temperatura effettiva di stelle giovani\, utili
zzando variabili fotometriche di stelle ottenute da tre cataloghi differen
ti\, ovvero Gaia\, Gaia-ESO Survey\, Pan-STARRS e 2MASS. I risultati previ
sivi evidenziano come il Random Forest rappresenti una buona soluzione per
la previsione della temperatura effettiva. Durante questo seminario intro
durro’ i cinque approcci statistici applicati nell’analisi svolta\, eviden
ziando in particolare i risultati relativi al Random Forest\, risultato il
migliore dei cinque.
DTSTART;TZID=Europe/Rome:20231004T120000
DTEND;TZID=Europe/Rome:20231004T133000
SEQUENCE:0
SUMMARY:Seminario: presentazione della tesi di Marco Tarantino (UNIPA)\, Au
la ore 12
URL:http://www.astropa.inaf.it/evento/seminario-presentazione-della-tesi-di
-marco-tarantino-unipa-aula-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Marco Tarantino Studente Magistrale in Sta
tistica e Data Science (LM-82)\, Universita’ degli Studi di Palermo
\n
Titolo:
\nAPPLICAZIONE DI TECNICHE STATISTICHE PER LA PREVISIONE D
ELLA
\nTEMPERATURA EFFETTIVA DI STELLE GIOVANI
\nAbstract:
\nUno degli attuali argomenti di discussione riguarda la durata del proce
sso di formazione di cluster stellari: vi sono modelli teorici che ipotizz
ano un unico evento dal quale si formano tutte le stelle appartenenti ad u
no stesso cluster\, considerando un processo di formazione rapido\, altri
modelli che\, invece\, suppongono piu’ eventi di formazione\, tenendo cont
o di un processo di formazione lento. Uno dei metodi piu’ utilizzati per r
icavare l’eta’ delle stelle si basa sul confronto della distribuzione dell
e stelle sul diagramma H-R con le isocrone teoriche. Una variabile fondame
ntale per applicare questo metodo e’ la temperatura efficace\, la quale s
i puo’ ricavare in maniera accurata dalla spettroscopia. Tuttavia\, nell’
epoca delle grandi survey fotometriche\, e’ necessario derivare la tempera
tura efficace basandosi sulla fotometria. L’obiettivo del lavoro consiste
nel trovare un modello che permetta di ottenere buone previsioni della tem
peratura effettiva di stelle giovani\, utilizzando variabili fotometriche
di stelle ottenute da tre cataloghi differenti\, ovvero Gaia\, Gaia-ESO Su
rvey\, Pan-STARRS e 2MASS. I risultati previsivi evidenziano come il Rando
m Forest rappresenti una buona soluzione per la previsione della temperatu
ra effettiva. Durante questo seminario introdurro’ i cinque approcci stati
stici applicati nell’analisi svolta\, evidenziando in particolare i risult
ati relativi al Random Forest\, risultato il migliore dei cinque.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26225@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:GIUSEPPE SCOZZARO\; giuseppe.scozzaro@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231005T143000
DTEND;TZID=Europe/Rome:20231005T163000
SEQUENCE:0
SUMMARY:RIUNIONE PNRR OAPa
URL:http://www.astropa.inaf.it/evento/riunione-pnrr-oapa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26239@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Giorgio La Malfa\nRelatore: Marco Miceli\nTitolo:Aniso
tropies in core-collapse supernova explosions: modeling the evolution of a
magnetorotational supernova remnant\nAbstract:\nThe core-collapse superno
vae (CCSNe) whose explosion is driven by mag-\nnetorotational instabilitie
s (MRIs) are believed to be viable sources of extremely\ninteresting astro
physical phenomena\, such as hypernovae\, super-luminous SNe\, magnetars a
nd gamma-ray bursts. Observations of the supernova remnants (SNRs) resulti
ng from these objects pose an important tool for their study. To this end\
,\nnumerical simulations offer valuable insights.\nHere my goal is to inve
stigate to which extent the supernova remnant (SNR)\nof an MR-SN retains m
emory of the explosion asymmetry\, and to study the mor-\nphology of the s
tellar ejecta throughout the evolution.\nI performed a three-dimensional (
3D) hydrodynamic (HD) simulation of a MR-\nSNR\, by evolving a state-of-th
e art MR-SN model available in the literature. The\nsimulation covers from
a few hours after the shock breakout to ∼ 10\,000 yrs\, with\nthe adoptio
n of an analytically prescribed circumstellar medium (CSM).\nThe early out
flow jet-like asymmetry\, characteristic of MR-SNe\, causes the for-\nmati
on of a Mach disk in the equatorial plane. This turns into a torus-like hi
gh\npressure region and leads the SNR to a bicone morphology. The pristine
bipolar\njet-like structure shows an asymmetry in the ejection time. The
simulation indi-\ncates that the remnant keeps memory of this asymmetry\,
presenting a narrower\nmorphology in the direction of the first ejected je
t. The forward shock presents\nan elongated morphology\, with a polar-to-e
quatorial ratio of ∼ 1.12 for the first ∼\n200 yrs\, decaying quite rapidl
y (down to ∼ 1.06) at ∼ 500 yrs. The stellar ejecta\nexhibit a higher rati
o of up to 1.20. The ejecta asymmetry increases when they\nextend to the f
orward shock through RT instabilities\, deforming the shock since\n∼ 200 y
rs. A comparison between a proxy of the X-ray emission and an X-ray\nChand
ra observation of Kes 73 (a SNR hosting a magnetar) indicates some simi-\n
larities\, though a more accurate treatment of the CSM could significantly
improve\nthe agreement with observations.\nThis first glimpse into the ev
olution of anisotropies in SNRs originating from\nMR-SNe indicates that th
e SNR keeps memory of the anisotropies in the MR ex-\nplosion on a time sc
ale of centuries\, rather than millenia.
DTSTART;TZID=Europe/Rome:20231005T150000
DTEND;TZID=Europe/Rome:20231005T163000
SEQUENCE:0
SUMMARY:Seminario: presentazione Tesi G. La Malfa (UNIPA)
URL:http://www.astropa.inaf.it/evento/seminario-presentazione-tesi-g-la-mal
fa-unipa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Giorgio La Malfa
\nRelatore: Marco Mi
celi
\nTitolo:Anisotropies in core-collapse supernova explosions: mod
eling the evolution of a magnetorotational supernova remnant
\nAbstra
ct:
\nThe core-collapse supernovae (CCSNe) whose explosion is driven
by mag-
\nnetorotational instabilities (MRIs) are believed to be viab
le sources of extremely
\ninteresting astrophysical phenomena\, such
as hypernovae\, super-luminous SNe\, magnetars and gamma-ray bursts. Obser
vations of the supernova remnants (SNRs) resulting from these objects pose
an important tool for their study. To this end\,
\nnumerical simulat
ions offer valuable insights.
\nHere my goal is to investigate to whi
ch extent the supernova remnant (SNR)
\nof an MR-SN retains memory of
the explosion asymmetry\, and to study the mor-
\nphology of the ste
llar ejecta throughout the evolution.
\nI performed a three-dimension
al (3D) hydrodynamic (HD) simulation of a MR-
\nSNR\, by evolving a s
tate-of-the art MR-SN model available in the literature. The
\nsimula
tion covers from a few hours after the shock breakout to ∼ 10\,000 yrs\, w
ith
\nthe adoption of an analytically prescribed circumstellar medium
(CSM).
\nThe early outflow jet-like asymmetry\, characteristic of MR
-SNe\, causes the for-
\nmation of a Mach disk in the equatorial plan
e. This turns into a torus-like high
\npressure region and leads the
SNR to a bicone morphology. The pristine bipolar
\njet-like structure
shows an asymmetry in the ejection time. The simulation indi-
\ncate
s that the remnant keeps memory of this asymmetry\, presenting a narrower<
br />\nmorphology in the direction of the first ejected jet. The forward s
hock presents
\nan elongated morphology\, with a polar-to-equatorial
ratio of ∼ 1.12 for the first ∼
\n200 yrs\, decaying quite rapidly (d
own to ∼ 1.06) at ∼ 500 yrs. The stellar ejecta
\nexhibit a higher ra
tio of up to 1.20. The ejecta asymmetry increases when they
\nextend
to the forward shock through RT instabilities\, deforming the shock since<
br />\n∼ 200 yrs. A comparison between a proxy of the X-ray emission and a
n X-ray
\nChandra observation of Kes 73 (a SNR hosting a magnetar) in
dicates some simi-
\nlarities\, though a more accurate treatment of t
he CSM could significantly improve
\nthe agreement with observations.
\nThis first glimpse into the evolution of anisotropies in SNRs orig
inating from
\nMR-SNe indicates that the SNR keeps memory of the anis
otropies in the MR ex-
\nplosion on a time scale of centuries\, rathe
r than millenia.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26287@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:francesca.martines@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231010T110000
DTEND;TZID=Europe/Rome:20231010T123000
SEQUENCE:0
SUMMARY:Riunione per lavori al Museo
URL:http://www.astropa.inaf.it/evento/riunione-per-lavori-al-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26226@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231011T140000
DTEND;TZID=Europe/Rome:20231011T193000
SEQUENCE:0
SUMMARY:Sketchtour in OAPA
URL:http://www.astropa.inaf.it/evento/sketchtour-in-oapa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26213@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Mario Guarcello (INAF)\nTitolo: “EWOCS: status of the
project.”\nAbstract: “The EWOCS project has the objective of studying star
and planet formation\, and early stellar evolution\, in very young massiv
e clusters (VYMCs). With a mass in excess of 10^4 solar masses\, the very
few VYMCs known in the Milky Way represent the most accessible examples of
starburst regions\, which are very rare in our Galaxy today\, but common
in galaxies experiencing epochs of intense star formation. These regions a
re characterized by very high stellar density\, and they are dominated by
a rich and compact ensemble of massive stars that produce an environment d
ominated by energetic radiation and particles. With a distance of 3.87 kpc
and 4.5 kpc\, respectively\, the Westerlund 1 and 2 clusters are the clos
est VYMCs to the Sun\, and thus the best targets to study how stars and pl
anets form in the most energetic star forming environment known. In this t
alk\, I will present the status and the preliminary results of the EWOCS p
roject\, which is mainly based on a 1Msec Chandra/ACIS-I Large Project and
a cycle 1 JWST observation of Westerlund 1\, a cycle 2 JWST observation o
f Westerlund 2\, and other data at high spatial resolution of the two clus
ters.”\nGoogle meet: https://meet.google.com/sxz-cctp-tsc?pli=1&authuser=1
DTSTART;TZID=Europe/Rome:20231012T150000
DTEND;TZID=Europe/Rome:20231012T163000
SEQUENCE:0
SUMMARY:Seminario: Mario Guarcello (INAF)\, ore 15
URL:http://www.astropa.inaf.it/evento/seminario-mario-guarcello-inaf-ore-15
/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Mario Guarcello (INAF)
\nTitolo: “EW
OCS: status of the project.”
\nAbstract: “The EWOCS project has the
objective of studying star and planet formation\, and early stellar evolut
ion\, in very young massive clusters (VYMCs). With a mass in excess of 10^
4 solar masses\, the very few VYMCs known in the Milky Way represent the m
ost accessible examples of starburst regions\, which are very rare in our
Galaxy today\, but common in galaxies experiencing epochs of intense star
formation. These regions are characterized by very high stellar density\,
and they are dominated by a rich and compact ensemble of massive stars tha
t produce an environment dominated by energetic radiation and particles. W
ith a distance of 3.87 kpc and 4.5 kpc\, respectively\, the Westerlund 1 a
nd 2 clusters are the closest VYMCs to the Sun\, and thus the best targets
to study how stars and planets form in the most energetic star forming en
vironment known. In this talk\, I will present the status and the prelimin
ary results of the EWOCS project\, which is mainly based on a 1Msec Chandr
a/ACIS-I Large Project and a cycle 1 JWST observation of Westerlund 1\, a
cycle 2 JWST observation of Westerlund 2\, and other data at high spatial
resolution of the two clusters.”
\nGoogle meet: https://meet.google.
com/sxz-cctp-tsc?pli=1&authuser=1
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-25901@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231017T100000
DTEND;TZID=Europe/Rome:20231017T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-5/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26180@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Maria Kopsacheili (ICE-CSIC)\nTitolo: New larger sampl
e of Supernova Remnants in NGC 7793\, using MUSE IFS.\nAbstract: Study of
Supernova Remnant (SNR) demographics and their physical properties (densit
y\, temperature\, shock velocities) is very important in order to understa
nd their role in galaxies. Many photometric and spectroscopic studies of S
NRs have been carried out in our Galaxy but also in extragalactic environm
ents. The most common means for the SNR identification in the optical regi
me\, is the use of the flux ratio of the [S II] (λλ6717\, 6731) to Hα (λ65
63) emission lines. However\, this diagnostic is biased against low excita
tion SNRs. For this reason\, we have developed new diagnostics that combin
e 2 and 3 emission line ratios along with a Support Vector Machine model\,
that efficiently differentiate SNRs from HII regions. These diagnostics r
ecover up to 35% of the SNRs that we miss using the traditional diagnostic
tool\, which is very important in order to obtain more complete samples o
f SNRs (i.e. SNRs of different physical properties) and consequently to mo
re efficiently explore the feedback processes to the host galaxy. We prese
nt the application of these diagnostics on Integral Field Unit (IFU) data
of the galaxy NGC 7793. We identify new SNR populations\, we construct the
distributions of their physical properties and their luminosity functions
. Finally\, we explore possible correlations between properties of SNRs an
d those of their environment.
DTSTART;TZID=Europe/Rome:20231018T150000
DTEND;TZID=Europe/Rome:20231018T163000
SEQUENCE:0
SUMMARY:Seminario: Maria Kopsacheili (ICE-CSIC)\, Aula ore 15
URL:http://www.astropa.inaf.it/evento/seminario-maria-kopsacheili-ice-csic-
aula-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Maria Kopsacheili (ICE-CSIC)
\nTitolo
: New larger sample of Supernova Remnants in NGC 7793\, using MUSE IFS.
\nAbstract: Study of Supernova Remnant (SNR) demographics and their phy
sical properties (density\, temperature\, shock velocities) is very import
ant in order to understand their role in galaxies. Many photometric and sp
ectroscopic studies of SNRs have been carried out in our Galaxy but also i
n extragalactic environments. The most common means for the SNR identifica
tion in the optical regime\, is the use of the flux ratio of the [S II] (λ
λ6717\, 6731) to Hα (λ6563) emission lines. However\, this diagnostic is b
iased against low excitation SNRs. For this reason\, we have developed new
diagnostics that combine 2 and 3 emission line ratios along with a Suppor
t Vector Machine model\, that efficiently differentiate SNRs from HII regi
ons. These diagnostics recover up to 35% of the SNRs that we miss using th
e traditional diagnostic tool\, which is very important in order to obtain
more complete samples of SNRs (i.e. SNRs of different physical properties
) and consequently to more efficiently explore the feedback processes to t
he host galaxy. We present the application of these diagnostics on Integra
l Field Unit (IFU) data of the galaxy NGC 7793. We identify new SNR popula
tions\, we construct the distributions of their physical properties and th
eir luminosity functions. Finally\, we explore possible correlations betwe
en properties of SNRs and those of their environment.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26346@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231107T100000
DTEND;TZID=Europe/Rome:20231107T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-6/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26292@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Emanuele Greco (INAF)\nTitolo: Jitter radiation as an
alternative for the nonthermal filaments in Supernova Remnants\nAbstract:
Synchrotron radiation from relativistic electrons is usually invoked as th
e responsible for the nonthermal emission observed in Supernova Remnants (
SNRs). Diffusive shock acceleration (DSA) is the most popular mechanism to
explain the process of particles acceleration and within its framework a
crucial role is played by the turbulent magnetic-field. However\, the stan
dard models commonly used to fit X-ray synchrotron emission do not take in
to account the effects of turbulence in the shape of the resulting photon
spectra. An alternative mechanism that properly includes such effects is t
he jitter radiation\, that provides for an additional power-law beyond the
classical synchrotron cutoff. In this talk\, i will show the results of a
pplying the jitter spectral model to various X-ray observations of Cassiop
eia A and found that it describes the X-ray soft-to-hard range better than
any of the standard cutoff models. I will also show what relevant turbule
nce and electrons’ parameters can be measured from the spectra in the jitt
er radiation framework.
DTSTART;TZID=Europe/Rome:20231109T160000
DTEND;TZID=Europe/Rome:20231109T170000
SEQUENCE:0
SUMMARY:Seminario: Emanuele Greco (INAF)\, Aula ore 16
URL:http://www.astropa.inaf.it/evento/seminario-emanuele-greco-inaf-aula-or
e-16/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Emanuele Greco (INAF)
\nTitolo: Jitte
r radiation as an alternative for the nonthermal filaments in Supernova Re
mnants
\nAbstract: Synchrotron radiation from relativistic electrons
is usually invoked as the responsible for the nonthermal emission observed
in Supernova Remnants (SNRs). Diffusive shock acceleration (DSA) is the m
ost popular mechanism to explain the process of particles acceleration and
within its framework a crucial role is played by the turbulent magnetic-f
ield. However\, the standard models commonly used to fit X-ray synchrotron
emission do not take into account the effects of turbulence in the shape
of the resulting photon spectra. An alternative mechanism that properly in
cludes such effects is the jitter radiation\, that provides for an additio
nal power-law beyond the classical synchrotron cutoff. In this talk\, i wi
ll show the results of applying the jitter spectral model to various X-ray
observations of Cassiopeia A and found that it describes the X-ray soft-t
o-hard range better than any of the standard cutoff models. I will also sh
ow what relevant turbulence and electrons’ parameters can be measured from
the spectra in the jitter radiation framework.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26371@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Ricevimento studenti\,Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231110T140000
DTEND;TZID=Europe/Rome:20231110T180000
SEQUENCE:0
SUMMARY:Visita studenti IC “Francesco Minà Palumbo” – Castelbuono
URL:http://www.astropa.inaf.it/evento/visita-studenti-ic-francesco-mina-pal
umbo-castelbuono/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26644@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Antonino Petralia
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231113T100000
DTEND;TZID=Europe/Rome:20231113T130000
SEQUENCE:0
SUMMARY:WG Machine Learning EXOPA
URL:http://www.astropa.inaf.it/evento/wg-machine-learning-exopa-3-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26260@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Marco Barbera\; +39 3346399413\; marco.barbera@unipa.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231114T090000
DTEND;TZID=Europe/Rome:20231114T173000
SEQUENCE:0
SUMMARY:Test Readiness Review – Contratto ESA “Fully Carbon Filters”
URL:http://www.astropa.inaf.it/evento/test-readiness-review-contratto-esa-f
ully-carbon-filters/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26293@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Speaker: Konstantina Anastasopoulou (INAF)\nTitolo: EWOCS: The
X-ray properties of the Wolf-Rayet stars in the young massive star cluster
Westerlund 1\nAbstract: Wolf-Rayet (WR) stars are the latest stage in the
evolution of very massive stars\, before they finally explode as supernov
ae (SN) or possibly gamma-ray bursts. They exhibit dense and powerful stel
lar winds that\, along with their ultimate death as core-collapse SN\, dom
inate the feedback to the local interstellar medium in star-forming galaxi
es. Studying in more detail the properties of the short-lived WR phase\, w
ill advance our understanding on star-formation processes and will test st
ellar evolutionary predictions. The best laboratory to study the WR phase
is the massive young star cluster Westerlund 1. It is the closest massive
star cluster to the Sun\, and it contains an impressive large sample of co
eval massive stars including the largest population (24) of WR stars in ou
r Galaxy. In this talk\, I will present the first results of the EWOCS (E
xtended Westerlund 1 and 2 Open Clusters Survey) project on the WR stars i
n Westerlund 1 based on a 1Msec Chandra/ACIS-I Large Project. With this ve
ry deep Chandra survey we are able to unravel the X-ray spectral\, colour\
, and timing properties of the entire WR population and retrieve insights
on their X-ray production mechanism. I will discuss these results in the c
ontext of different spectral subtypes of WR stars\, as well as binarity si
nce the majority of them show clear signs of very hot plasma created in th
e colliding-wind region of a binary system.
DTSTART;TZID=Europe/Rome:20231115T150000
DTEND;TZID=Europe/Rome:20231115T163000
SEQUENCE:0
SUMMARY:Seminario: Konstantina Anastasopoulou (INAF)\, Aula ore 15
URL:http://www.astropa.inaf.it/evento/seminario-konstantina-anastasopoulou-
inaf-aula-ore-15/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Konstantina Anastasopoulou (INAF)
\nT
itolo: EWOCS: The X-ray properties of the Wolf-Rayet stars in the young ma
ssive star cluster Westerlund 1
\nAbstract: Wolf-Rayet (WR) stars ar
e the latest stage in the evolution of very massive stars\, before they fi
nally explode as supernovae (SN) or possibly gamma-ray bursts. They exhibi
t dense and powerful stellar winds that\, along with their ultimate death
as core-collapse SN\, dominate the feedback to the local interstellar medi
um in star-forming galaxies. Studying in more detail the properties of the
short-lived WR phase\, will advance our understanding on star-formation p
rocesses and will test stellar evolutionary predictions. The best laborato
ry to study the WR phase is the massive young star cluster Westerlund 1. I
t is the closest massive star cluster to the Sun\, and it contains an impr
essive large sample of coeval massive stars including the largest populati
on (24) of WR stars in our Galaxy. In this talk\, I will present the first
results of the EWOCS (Extended Westerlund 1 and 2 Open Clusters Survey)
project on the WR stars in Westerlund 1 based on a 1Msec Chandra/ACIS-I La
rge Project. With this very deep Chandra survey we are able to unravel the
X-ray spectral\, colour\, and timing properties of the entire WR populati
on and retrieve insights on their X-ray production mechanism. I will discu
ss these results in the context of different spectral subtypes of WR stars
\, as well as binarity since the majority of them show clear signs of very
hot plasma created in the colliding-wind region of a binary system.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26670@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231122T110000
DTEND;TZID=Europe/Rome:20231122T130000
SEQUENCE:0
SUMMARY:Riunione gruppo SNR
URL:http://www.astropa.inaf.it/evento/riunione-gruppo-snr-5/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26231@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231127T150000
DTEND;TZID=Europe/Rome:20231127T170000
SEQUENCE:0
SUMMARY:Riunione HPC (SCAN)
URL:http://www.astropa.inaf.it/evento/riunione-hpc-scan-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26504@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231128T100000
DTEND;TZID=Europe/Rome:20231128T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-7/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26661@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Formazione\,Aula: Riunione
CONTACT:GIUSEPPE SCOZZARO
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231128T140000
DTEND;TZID=Europe/Rome:20231128T183000
SEQUENCE:0
SUMMARY:CORSO DI FORMAZIONE AFFIDAMENTI GARE PNRR @aula piazzi
URL:http://www.astropa.inaf.it/evento/corso-di-formazione-affidamenti-gare-
pnrr/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26662@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Formazione\,Aula: Riunione
CONTACT:giuseppe scozzaro
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231129T093000
DTEND;TZID=Europe/Rome:20231129T170000
SEQUENCE:0
SUMMARY:CORSO DI FORMAZIONE AFFIDAMENTI GARE PNRR @aula piazzi
URL:http://www.astropa.inaf.it/evento/corso-di-formazione-affidamenti-gare-
pnrr-aula-piazzi/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26663@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Formazione\,Aula: Riunione
CONTACT:giuseppe scozzaro
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231130T093000
DTEND;TZID=Europe/Rome:20231130T170000
SEQUENCE:0
SUMMARY:CORSO DI FORMAZIONE AFFIDAMENTI GARE PNRR @aula piazzi
URL:http://www.astropa.inaf.it/evento/corso-di-formazione-affidamenti-gare-
pnrr-aula-piazzi-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26380@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Kevin France (University of Colorado at Boulder)\nTitl
e: Exploring Extreme Exoplanets and Stellar Activity with Small Satellite
Missions\nAbstract: Atmospheric escape is a process that affects the stru
cture\, composition\, and evolution of many planets. Atmospheric escape r
ates depend critically on the extreme-ultraviolet (EUV) and far-ultraviole
t (FUV) photon fluxes from the host star. Owing to high levels of EUV and
FUV irradiance from their nearby parent stars\, the signatures of rapid a
tmospheric escape are detectable on close-in\, gaseous exoplanets transiti
ng bright stars. In this talk\, I will present current and future small s
atellite missions designed to directly observe atmospheric escape from exo
planets and to investigate the EUV luminosity and energy partition of EUV
flares on nearby stars. The majority of the talk will focus on the Colorad
o Ultraviolet Transit Experiment (CUTE)\, a 6U CubeSat mission designed to
take advantage of the near-ultraviolet (250 – 330 nm) stellar brightness
distribution to conduct novel observations of the extended atmospheres of
nearby close-in planets. CUTE is NASA’s first dedicated exoplanet spectro
scopy mission and has collected 6 – 11 transits of each of seven short-per
iod exoplanets. I will present an overview of the CUTE mission\, includin
g its development path and on-orbit observations of excess NUV absorption
on ultra-hot Jupiters. I will conclude the talk by describing the upcomin
g Monitoring Activity from Nearby sTars with uv Imaging and Spectroscopy (
MANTIS) mission\, a 12U CubeSat that will make simultaneous observations o
f nearby stars in four spectral bands from the EUV through the optical (~1
0 – 1000 nm). MANTIS will conduct two surveys over its planned two-year m
ission lifetime: deep EUV observations of nearby stars and contemporaneous
stellar characterization data in support of James Webb Space Telescope ex
oplanet spectroscopy observations.
DTSTART;TZID=Europe/Rome:20231201T120000
DTEND;TZID=Europe/Rome:20231201T130000
SEQUENCE:0
SUMMARY:Seminario: Kevin France (University of Colorado at Boulder)\, Aula
ore 12
URL:http://www.astropa.inaf.it/evento/seminario-kevin-france-university-of-
colorado-at-boulder-aula-ore-12/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Kevin France (University of Colorado at Bo
ulder)
\nTitle: Exploring Extreme Exoplanets and Stellar Activity w
ith Small Satellite Missions
\nAbstract: Atmospheric escape is a pro
cess that affects the structure\, composition\, and evolution of many plan
ets. Atmospheric escape rates depend critically on the extreme-ultraviole
t (EUV) and far-ultraviolet (FUV) photon fluxes from the host star. Owing
to high levels of EUV and FUV irradiance from their nearby parent stars\,
the signatures of rapid atmospheric escape are detectable on close-in\, g
aseous exoplanets transiting bright stars. In this talk\, I will present
current and future small satellite missions designed to directly observe a
tmospheric escape from exoplanets and to investigate the EUV luminosity an
d energy partition of EUV flares on nearby stars. The majority of the talk
will focus on the Colorado Ultraviolet Transit Experiment (CUTE)\, a 6U C
ubeSat mission designed to take advantage of the near-ultraviolet (250 – 3
30 nm) stellar brightness distribution to conduct novel observations of th
e extended atmospheres of nearby close-in planets. CUTE is NASA’s first d
edicated exoplanet spectroscopy mission and has collected 6 – 11 transits
of each of seven short-period exoplanets. I will present an overview of t
he CUTE mission\, including its development path and on-orbit observations
of excess NUV absorption on ultra-hot Jupiters. I will conclude the talk
by describing the upcoming Monitoring Activity from Nearby sTars with uv
Imaging and Spectroscopy (MANTIS) mission\, a 12U CubeSat that will make s
imultaneous observations of nearby stars in four spectral bands from the E
UV through the optical (~10 – 1000 nm). MANTIS will conduct two surveys o
ver its planned two-year mission lifetime: deep EUV observations of nearby
stars and contemporaneous stellar characterization data in support of Jam
es Webb Space Telescope exoplanet spectroscopy observations.
\n<
/HTML>
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26413@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231201T140000
DTEND;TZID=Europe/Rome:20231201T180000
SEQUENCE:0
SUMMARY:MANTIS science team
URL:http://www.astropa.inaf.it/evento/mantis-science-team/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26582@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Referente: Ileana Chinnici
DTSTART;TZID=Europe/Rome:20231201T164500
DTEND;TZID=Europe/Rome:20231201T184500
SEQUENCE:0
SUMMARY:Visita al Museo
URL:http://www.astropa.inaf.it/evento/visita-al-museo-7/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nReferente: Ileana Chinnici
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26744@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Aula: Seminario\,Aula: Teleconfer
enza
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231204T153000
DTEND;TZID=Europe/Rome:20231204T163000
SEQUENCE:0
SUMMARY:INCONTRO ONLINE TRA MONIA ROSSI CANDIDATA CDA INAF ED I DIPENDENTI
URL:http://www.astropa.inaf.it/evento/incontro-online-tra-monia-rossi-candi
data-cda-inaf-ed-i-dipendenti/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26748@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231205T100000
DTEND;TZID=Europe/Rome:20231205T193000
SEQUENCE:0
SUMMARY:Collegio dei Direttori al Museo
URL:http://www.astropa.inaf.it/evento/collegio-dei-direttori-al-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26747@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:Pranzo Collegio dei direttori
DTSTART;TZID=Europe/Rome:20231205T120000
DTEND;TZID=Europe/Rome:20231205T150000
SEQUENCE:0
SUMMARY:Pranzo Collegio dei direttori
URL:http://www.astropa.inaf.it/evento/pranzo-collegio-dei-direttori/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nPranzo Collegio dei direttori
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26681@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231206T110000
DTEND;TZID=Europe/Rome:20231206T130000
SEQUENCE:0
SUMMARY:Incontro di A.Comastri con il personale OAPa
URL:http://www.astropa.inaf.it/evento/incontro-di-a-comastri-con-il-persona
le-oapa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26761@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231211T163000
DTEND;TZID=Europe/Rome:20231211T183000
SEQUENCE:0
SUMMARY:Visita al Museo
URL:http://www.astropa.inaf.it/evento/visita-al-museo-8/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26736@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231212T100000
DTEND;TZID=Europe/Rome:20231212T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-8/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26760@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231212T110000
DTEND;TZID=Europe/Rome:20231212T150000
RDATE;TZID=Europe/Rome:20231212T110000
RDATE;TZID=Europe/Rome:20231213T110000
RDATE;TZID=Europe/Rome:20231215T110000
SEQUENCE:0
SUMMARY:Revisione schede conservazione dei beni del Museo
URL:http://www.astropa.inaf.it/evento/revisione-schede-conservazione-dei-be
ni-del-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26647@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Francesca Martines\; francesca.martines@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231219T090000
DTEND;TZID=Europe/Rome:20231219T130000
LOCATION:Museo
SEQUENCE:0
SUMMARY:Visita classe scolastica per biblioteca\, archivio e museo
URL:http://www.astropa.inaf.it/evento/visita-classe-scolastica-per-bibliote
ca-archivio-e-museo/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26844@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231219T100000
DTEND;TZID=Europe/Rome:20231219T110000
SEQUENCE:0
SUMMARY:Riunione SOC Scuola 3d-ASTROPA II
URL:http://www.astropa.inaf.it/evento/riunione-soc-scuola-3d-astropa-ii/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26684@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:Francesca Martines\; francesca.martines@ginaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20231220T100000
DTEND;TZID=Europe/Rome:20231220T123000
SEQUENCE:0
SUMMARY:Visita studenti di Architettura
URL:http://www.astropa.inaf.it/evento/visita-studenti-di-architettura/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26896@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Ileana Chinnici (INAF)\nTitolo:Piazzi\, Fratelli murat
ori\, logge e documenti massonici\nAbstract: TBD
DTSTART;TZID=Europe/Rome:20231228T093500
DTEND;TZID=Europe/Rome:20231228T103500
SEQUENCE:0
SUMMARY:Seminario: Ileana Chinnici (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-ileana-chinnici-inaf-5/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Ileana Chinnici (INAF)
\nTitolo:Piazz
i\, Fratelli muratori\, logge e documenti massonici
\nAbstract: TBD
p>\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26680@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240110T150000
DTEND;TZID=Europe/Rome:20240110T163000
SEQUENCE:0
SUMMARY:Riunione HPC
URL:http://www.astropa.inaf.it/evento/riunione-hpc/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n
\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26937@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240111T110000
DTEND;TZID=Europe/Rome:20240111T120000
SEQUENCE:0
SUMMARY:riunione (Angela)
URL:http://www.astropa.inaf.it/evento/riunione-angela/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26967@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240115T110000
DTEND;TZID=Europe/Rome:20240115T130000
SEQUENCE:0
SUMMARY:CdS
URL:http://www.astropa.inaf.it/evento/cds/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26872@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:Meeting exopa\, normalmente in aula. Se l’aula sarà occupata a
causa dei lavori in amministrazione \, il meeting si svolgerà al museo
DTSTART;TZID=Europe/Rome:20240116T100000
DTEND;TZID=Europe/Rome:20240116T130000
SEQUENCE:0
SUMMARY:meeting exopa
URL:http://www.astropa.inaf.it/evento/meeting-exopa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nMeeting exopa\, normalmente in aula. Se l’aula sarà
occupata a causa dei lavori in amministrazione \, il meeting si svolgerà
al museo
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27007@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240124T110000
DTEND;TZID=Europe/Rome:20240124T120000
SEQUENCE:0
SUMMARY:Sopralluogo per performance teatrale
URL:http://www.astropa.inaf.it/evento/sopralluogo-per-performance-teatrale/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26985@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240124T150000
DTEND;TZID=Europe/Rome:20240124T163000
SEQUENCE:0
SUMMARY:Riunione SNR@OAPa
URL:http://www.astropa.inaf.it/evento/riunione-snroapa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26984@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240125T110000
DTEND;TZID=Europe/Rome:20240125T130000
SEQUENCE:0
SUMMARY:M dwarfs meeting
URL:http://www.astropa.inaf.it/evento/m-dwarfs-meeting/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27016@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Sara Bonito\; rosaria.bonito@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240126T120000
DTEND;TZID=Europe/Rome:20240126T130000
SEQUENCE:0
SUMMARY:Riunione LIS e Giornata Internazionale delle Donne e delle Ragazze
nella Scienza
URL:http://www.astropa.inaf.it/evento/riunione-lis-e-giornata-internazional
e-delle-donne-e-delle-ragazze-nella-scienza/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26972@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Museo
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240130T100000
DTEND;TZID=Europe/Rome:20240130T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-9/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27049@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Aula: Teleconferenza
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240131T110000
DTEND;TZID=Europe/Rome:20240131T130000
SEQUENCE:0
SUMMARY:Riunione correlazione pianeta-metallicità
URL:http://www.astropa.inaf.it/evento/riunione-correlazione-pianeta-metalli
cita/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27059@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Aula: Teleconferenza
CONTACT:filippo salemi
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240201T114500
DTEND;TZID=Europe/Rome:20240201T133000
SEQUENCE:0
SUMMARY:webinar appalti @aula piazzi
URL:http://www.astropa.inaf.it/evento/webinar-appalti/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27050@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240201T163000
DTEND;TZID=Europe/Rome:20240201T183000
SEQUENCE:0
SUMMARY:Visita al Museo Club Inner Wheel Palermo Normanna
URL:http://www.astropa.inaf.it/evento/visita-al-museo-club-inner-wheel-pale
rmo-normanna/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26286@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Concorso\,Museo
CONTACT:
DESCRIPTION:Ref. Daricello
DTSTART;TZID=Europe/Rome:20240207T133000
DTEND;TZID=Europe/Rome:20240207T190000
RDATE;TZID=Europe/Rome:20240208T133000
SEQUENCE:0
SUMMARY:Campionati di astronomia
URL:http://www.astropa.inaf.it/evento/campionati-di-astronomia/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nRef. Daricello
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27014@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240208T090000
DTEND;TZID=Europe/Rome:20240208T133000
SEQUENCE:0
SUMMARY:Prova performance teatrale
URL:http://www.astropa.inaf.it/evento/prova-performance-teatrale/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27005@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Museo
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240209T150000
DTEND;TZID=Europe/Rome:20240209T193000
SEQUENCE:0
SUMMARY:Performance teatrale
URL:http://www.astropa.inaf.it/evento/performance-teatrale/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27047@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240213T100000
DTEND;TZID=Europe/Rome:20240213T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-10/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27171@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240213T143000
DTEND;TZID=Europe/Rome:20240213T160000
SEQUENCE:0
SUMMARY:Incontro con U. Becciani su Bandi a cascata CN HPC
URL:http://www.astropa.inaf.it/evento/incontro-con-u-becciani-su-bandi-a-ca
scata-cn-hpc/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27175@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240216T093000
DTEND;TZID=Europe/Rome:20240216T133000
SEQUENCE:0
SUMMARY:Riunione Masse RV
URL:http://www.astropa.inaf.it/evento/riunione-masse-rv/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27190@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Aula: Teleconferenza
CONTACT:Sara Bonito\; rosaria.bonito@inaf.it
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240216T140000
DTEND;TZID=Europe/Rome:20240216T183000
SEQUENCE:0
SUMMARY:Congresso La vita e lo spazio (remoto): invited
URL:http://www.astropa.inaf.it/evento/congresso-la-vita-e-lo-spazio-remoto-
invited/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27135@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Francesco Malara (UniCal)\nTitolo del talk: “MHD waves
and turbulence in plasmas of the solar corona”\nAbstract:\n“The solar cor
ona is made of extremely tenuous plasmas having different physical conditi
ons\, e.g.\, temperature\, density\, and magnetic fields. In response to p
erturbations\, restoring forces determined by pressure and the local magne
tic field can determine the formation and propagation of magnetohydrodynam
ic (MHD) waves. Coronal loops sustain the propagation of different types o
f MHD with a broad range of periods and amplitude\, with the most easily o
bserved and studied one being the kink mode. Kink waves in loops\, usually
excited in impulsive events (e.g. flares) with amplitude of 4-5 Mm and pe
riods of 3-5 min\, are strongly damped within few wave periods. However\,
high-resolution observations from different space missions in the last dec
ade have shown the omnipresence of so-called “decayless fluctuations”\, i.
e.\, kink oscillations with a small amplitude (< 1 Mm) and no damping. The
ir discovery in the solar corona has posed new questions about their drive
r and the mechanisms for energy transfer in the solar atmosphere. In fact\
, the dissipation of the fluctuation energy is one of the possible mechani
sms that are believed to be resposible for the heating of the solar corona
. In an extremely high Reynolds/Lundquist number plasma\, such as in the c
orona\, a key role is played by fluctuation-inhomogeneity couplings\, as w
ell as by nonlinear effects that generate a turbulent cascade. In the last
few decades such effects have been studied in great detail. Here we prese
nt a numerical investigation aiming at clarifying the interplay of these t
wo mechanims in the dissipation of Alfvén waves. We find that\, in a regim
e representative of coronal magnetic structures\, fluctuation-inhomogeneit
y couplings and turbulence synergically work to significantly speed up the
conversion of fluctuating kinetic/magnetic energy into thermal energy. Th
eir potential contribution to solving the coronal heating problem is empha
sized\, as well as the potentialities offered by the MUSE mission in study
ing the formation and evolution of MHD waves in the corona.”
DTSTART;TZID=Europe/Rome:20240220T150000
DTEND;TZID=Europe/Rome:20240220T160000
SEQUENCE:0
SUMMARY:Seminario: Francesco Malara (UniCal)
URL:http://www.astropa.inaf.it/evento/seminario-francesco-malara-unical/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Francesco Malara (UniCal)
\nTitolo d
el talk: “MHD waves and turbulence in plasmas of the solar corona”
\nAbstract:
\n“The solar corona is made of extremely tenuous plasmas h
aving different physical conditions\, e.g.\, temperature\, density\, and m
agnetic fields. In response to perturbations\, restoring forces determined
by pressure and the local magnetic field can determine the formation and
propagation of magnetohydrodynamic (MHD) waves. Coronal loops sustain the
propagation of different types of MHD with a broad range of periods and am
plitude\, with the most easily observed and studied one being the kink mod
e. Kink waves in loops\, usually excited in impulsive events (e.g. flares)
with amplitude of 4-5 Mm and periods of 3-5 min\, are strongly damped wit
hin few wave periods. However\, high-resolution observations from differen
t space missions in the last decade have shown the omnipresence of so-call
ed “decayless fluctuations”\, i.e.\, kink oscillations with a small amplit
ude (< 1 Mm) and no damping. Their discovery in the solar corona has posed
new questions about their driver and the mechanisms for energy transfer i
n the solar atmosphere. In fact\, the dissipation of the fluctuation energ
y is one of the possible mechanisms that are believed to be resposible for
the heating of the solar corona. In an extremely high Reynolds/Lundquist
number plasma\, such as in the corona\, a key role is played by fluctuatio
n-inhomogeneity couplings\, as well as by nonlinear effects that generate
a turbulent cascade. In the last few decades such effects have been studie
d in great detail. Here we present a numerical investigation aiming at cla
rifying the interplay of these two mechanims in the dissipation of Alfvén
waves. We find that\, in a regime representative of coronal magnetic struc
tures\, fluctuation-inhomogeneity couplings and turbulence synergically wo
rk to significantly speed up the conversion of fluctuating kinetic/magneti
c energy into thermal energy. Their potential contribution to solving the
coronal heating problem is emphasized\, as well as the potentialities offe
red by the MUSE mission in studying the formation and evolution of MHD wav
es in the corona.”
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26891@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Ileana Chinnici (INAF)\nTitolo: Le spedizioni scientif
iche dell’Osservatorio di Palermo\, ieri e oggi\nAbstract:\nAnche l’Osserv
atorio di Palermo\, nel corso della sua lunga storia\, ha organizzato o pa
rtecipato ad alcune spedizioni scientifiche\; naturalmente\, non sempre si
è trattato di finalità vòlte a studi astronomici\, ma in ogni caso le spe
dizioni avevano scopi scientifici. Tra quelle di carattere astronomico van
no ricordate\, in particolare\, la spedizione nella Sicilia sud-orientale
per l’osservazione dell’eclisse totale di Sole del 1870\, quella per il tr
ansito di Venere in India nel 1874\, quella per le eclissi totale di Sole
nelle Isole Nicobar nel 1875 e in Tunisia nel 1905. Di recente\, come è no
to\, è stata anche organizzata una spedizione in Calabria per l’occultazio
ne di Betelgeuse da parte dell’asteroide Leonia nel dicembre 2023. Lo scop
o di questo seminario è quello di illustrare soprattutto le spedizioni sto
riche astronomiche (da cui sempre c’è da imparare!) e raccogliere notizie
su eventuali altre spedizioni del XX secolo di cui hanno memoria i collegh
i più anziani.
DTSTART;TZID=Europe/Rome:20240221T153000
DTEND;TZID=Europe/Rome:20240221T170000
SEQUENCE:0
SUMMARY:Seminario: Ileana Chinnici (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-ileana-chinnici-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Ileana Chinnici (INAF)
\nTitolo: Le s
pedizioni scientifiche dell’Osservatorio di Palermo\, ieri e oggi
\n
Abstract:
\nAnche l’Osservatorio di Palermo\, nel corso della sua lun
ga storia\, ha organizzato o partecipato ad alcune spedizioni scientifiche
\; naturalmente\, non sempre si è trattato di finalità vòlte a studi astro
nomici\, ma in ogni caso le spedizioni avevano scopi scientifici. Tra quel
le di carattere astronomico vanno ricordate\, in particolare\, la spedizio
ne nella Sicilia sud-orientale per l’osservazione dell’eclisse totale di S
ole del 1870\, quella per il transito di Venere in India nel 1874\, quella
per le eclissi totale di Sole nelle Isole Nicobar nel 1875 e in Tunisia n
el 1905. Di recente\, come è noto\, è stata anche organizzata una spedizio
ne in Calabria per l’occultazione di Betelgeuse da parte dell’asteroide Le
onia nel dicembre 2023. Lo scopo di questo seminario è quello di illustrar
e soprattutto le spedizioni storiche astronomiche (da cui sempre c’è da im
parare!) e raccogliere notizie su eventuali altre spedizioni del XX secolo
di cui hanno memoria i colleghi più anziani.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27194@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240222T113000
DTEND;TZID=Europe/Rome:20240222T130000
SEQUENCE:0
SUMMARY:Riunione CME
URL:http://www.astropa.inaf.it/evento/riunione-cme/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27193@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240222T150000
DTEND;TZID=Europe/Rome:20240222T163000
SEQUENCE:0
SUMMARY:Riunione Julien
URL:http://www.astropa.inaf.it/evento/riunione-julien/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27172@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240227T100000
DTEND;TZID=Europe/Rome:20240227T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-11/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27136@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Victor Almendros (INAF)\nTitle: Evolution of the mass
accretion rate and its relationship with the stellar and disk mass from br
own dwarfs to stars\nAbstract:\nThe time evolution of the dependence of th
e mass accretion rate with the stellar mass and the disk mass represents a
fundamental way to understand the evolution of protoplanetary disks and t
he formation of planets. Recent studies suggest the existence of a bimodal
accretion behavior at 2-3 Myr in the relationship of the stellar mass and
the mass accretion rate\, which may indicate that low-mass stars evolve f
aster (than higher-mass stars) into lower accretion rates. We recently mea
sured the mass accretion rate of 26 new brown dwarfs and low-mass stars in
the Ophiuchus\, Cha-I and Upper Scorpius star-forming regions using X-Sho
oter/VLT. Combining these new observations with data from the literature\,
we compared the relations between accretion rate and stellar/disk propert
ies of four different star-forming regions with different ages: Ophiuchus
(1 Mar)\, Lupus (2 Myr)\, Cha-I (3 Myr) and Upper Scorpius (5-12 Myr). Ove
rall\, we observe hints of a faster evolution into low accretion rates of
low-mass stars and brown dwarfs. At the same time\, we also found that bro
wn dwarfs present larger Mdisk/Macc ratios than stars in Ophiuchus\, Lupus
and Cha-I. This apparently contradictory result may imply that the evolut
ion of protoplanetary disks around brown dwarfs may be different than in t
he stellar regime.
DTSTART;TZID=Europe/Rome:20240227T150000
DTEND;TZID=Europe/Rome:20240227T163000
SEQUENCE:0
SUMMARY:Seminario: Victor Almendros (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-victor-almendros-inaf/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Victor Almendros (INAF)
\nTitle: Evo
lution of the mass accretion rate and its relationship with the stellar an
d disk mass from brown dwarfs to stars
\nAbstract:
\nThe time e
volution of the dependence of the mass accretion rate with the stellar mas
s and the disk mass represents a fundamental way to understand the evoluti
on of protoplanetary disks and the formation of planets. Recent studies su
ggest the existence of a bimodal accretion behavior at 2-3 Myr in the rela
tionship of the stellar mass and the mass accretion rate\, which may indic
ate that low-mass stars evolve faster (than higher-mass stars) into lower
accretion rates. We recently measured the mass accretion rate of 26 new br
own dwarfs and low-mass stars in the Ophiuchus\, Cha-I and Upper Scorpius
star-forming regions using X-Shooter/VLT. Combining these new observations
with data from the literature\, we compared the relations between accreti
on rate and stellar/disk properties of four different star-forming regions
with different ages: Ophiuchus (1 Mar)\, Lupus (2 Myr)\, Cha-I (3 Myr) an
d Upper Scorpius (5-12 Myr). Overall\, we observe hints of a faster evolut
ion into low accretion rates of low-mass stars and brown dwarfs. At the sa
me time\, we also found that brown dwarfs present larger Mdisk/Macc ratios
than stars in Ophiuchus\, Lupus and Cha-I. This apparently contradictory
result may imply that the evolution of protoplanetary disks around brown d
warfs may be different than in the stellar regime.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27261@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240228T110000
DTEND;TZID=Europe/Rome:20240228T130000
SEQUENCE:0
SUMMARY:M dwarfs meeting
URL:http://www.astropa.inaf.it/evento/m-dwarfs-meeting-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27285@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione\,Aula: Seminario\,Aula: Teleconfer
enza
CONTACT:GIUSEPPE SCOZZARO
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240229T140000
DTEND;TZID=Europe/Rome:20240229T150000
SEQUENCE:0
SUMMARY:RIUNIONE TIMESHEET PNRR TD
URL:http://www.astropa.inaf.it/evento/riunione-timesheet-pnrr-td/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27240@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240301T100000
DTEND;TZID=Europe/Rome:20240301T130000
SEQUENCE:0
SUMMARY:Machine Learning Gordon
URL:http://www.astropa.inaf.it/evento/machine-learning-gordon/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27290@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240305T090000
DTEND;TZID=Europe/Rome:20240305T110000
SEQUENCE:0
SUMMARY:Riunione gruppo SNR
URL:http://www.astropa.inaf.it/evento/riunione-gruppo-snr-6/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27295@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240306T090000
DTEND;TZID=Europe/Rome:20240306T133000
SEQUENCE:0
SUMMARY:MINERVA
URL:http://www.astropa.inaf.it/evento/minerva-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27291@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240312T100000
DTEND;TZID=Europe/Rome:20240312T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-12/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27335@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240314T100000
DTEND;TZID=Europe/Rome:20240314T123000
SEQUENCE:0
SUMMARY:M dwarfs meeting
URL:http://www.astropa.inaf.it/evento/m-dwarfs-meeting-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27404@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240318T120000
DTEND;TZID=Europe/Rome:20240318T130000
SEQUENCE:0
SUMMARY:Riunione LOC Ariel IT
URL:http://www.astropa.inaf.it/evento/riunione-loc-ariel-it/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26893@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Ileana Chinnici (INAF)\nTitolo: Tra i segreti di un ma
noscritto: lo strumento misterioso\nAbstrat: Un manoscritto nascosto\, una
lettera su E-bay\, uno strumento misterioso: sono gli ingredienti di un “
giallo”\, illustrato in questo seminario\, che ci riporterà alla fine del
Settecento\, tra sospetti\, dubbi e test sulla affidabilità degli strument
i utilizzati dagli astronomi inglesi. Per qualche (finora) oscuro motivo\,
l’Osservatorio di Palermo è entrato in possesso di un importante document
o relativo a tali questioni: lo studio di questo manoscritto ha rivelato l
’esistenza uno strumento sconosciuto\, di cui non si trova (quasi) traccia
.
DTSTART;TZID=Europe/Rome:20240321T150000
DTEND;TZID=Europe/Rome:20240321T163000
SEQUENCE:0
SUMMARY:Seminario: Ileana Chinnici (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-ileana-chinnici-inaf-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Ileana Chinnici (INAF)
\nTitolo: Tra
i segreti di un manoscritto: lo strumento misterioso
\nAbstrat: Un
manoscritto nascosto\, una lettera su E-bay\, uno strumento misterioso: so
no gli ingredienti di un “giallo”\, illustrato in questo seminario\, che c
i riporterà alla fine del Settecento\, tra sospetti\, dubbi e test sulla a
ffidabilità degli strumenti utilizzati dagli astronomi inglesi. Per qualch
e (finora) oscuro motivo\, l’Osservatorio di Palermo è entrato in possesso
di un importante documento relativo a tali questioni: lo studio di questo
manoscritto ha rivelato l’esistenza uno strumento sconosciuto\, di cui no
n si trova (quasi) traccia.
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27403@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240322T093000
DTEND;TZID=Europe/Rome:20240322T133000
SEQUENCE:0
SUMMARY:MINERVA
URL:http://www.astropa.inaf.it/evento/minerva-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27418@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Concorso\,Aula: Riunione\,Aula: Seminario
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240325T100000
DTEND;TZID=Europe/Rome:20240325T120000
SEQUENCE:0
SUMMARY:riunione amministrativa
URL:http://www.astropa.inaf.it/evento/riunione-amministrativa/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27347@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240326T100000
DTEND;TZID=Europe/Rome:20240326T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-13/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27419@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Concorso\,Aula: Esami\,Aula: Riunione
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240327T100000
DTEND;TZID=Europe/Rome:20240327T110000
SEQUENCE:0
SUMMARY:riunione amministrativa
URL:http://www.astropa.inaf.it/evento/riunione-amministrativa-2/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27399@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario\,Aula: Teleconferenza
CONTACT:
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240403T100000
DTEND;TZID=Europe/Rome:20240403T130000
SEQUENCE:0
SUMMARY:M dwarfs
URL:http://www.astropa.inaf.it/evento/massive-stars-collaboration-uam-cab/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-27426@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Riunione
CONTACT:Mattia D'Arpa
DESCRIPTION:
DTSTART;TZID=Europe/Rome:20240409T100000
DTEND;TZID=Europe/Rome:20240409T130000
SEQUENCE:0
SUMMARY:Riunione EXOPA
URL:http://www.astropa.inaf.it/evento/riunione-exopa-14/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26894@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Titolo: Carte geografiche\, tra arte e scienza (M. Coniglio\, I
. Chinnici)\nSpeaker: Ileana Chinnici (INAF)\nAbstract: TBD
DTSTART;TZID=Europe/Rome:20240411T150000
DTEND;TZID=Europe/Rome:20240411T163000
SEQUENCE:0
SUMMARY:Seminario: Manuela Coniglio e Ileana Chinnici (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-ileana-chinnici-inaf-3/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nTitolo: Carte geografiche\, tra arte e scienza (M.
Coniglio\, I. Chinnici)
\nSpeaker: Ileana Chinnici (INAF)
\nAb
stract: TBD
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26895@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Ileana Chinnici (INAF)\nTitolo: Il Cerchio di Ramsden\
, un prodigio tecnologico\nAbstract: TBD
DTSTART;TZID=Europe/Rome:20240516T150000
DTEND;TZID=Europe/Rome:20240516T163000
SEQUENCE:0
SUMMARY:Seminario: Ileana Chinnici (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-ileana-chinnici-inaf-4/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Ileana Chinnici (INAF)
\nTitolo: Il C
erchio di Ramsden\, un prodigio tecnologico
\nAbstract: TBD
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26897@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Ileana Chinnici (INAF)\nTitolo: Warning from Mars: il
restauro del globo di Marte del Museo della Specola\nAbstract: TBD
DTSTART;TZID=Europe/Rome:20240912T150000
DTEND;TZID=Europe/Rome:20240912T163000
SEQUENCE:0
SUMMARY:Seminario: Ileana Chinnici (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-ileana-chinnici-inaf-6/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Ileana Chinnici (INAF)
\nTitolo: Warn
ing from Mars: il restauro del globo di Marte del Museo della Specola
\nAbstract: TBD
\n
END:VEVENT
BEGIN:VEVENT
UID:ai1ec-26898@www.astropa.inaf.it
DTSTAMP:20240329T140515Z
CATEGORIES;LANGUAGE=it-IT:Aula: Seminario
CONTACT:
DESCRIPTION:Speaker: Ileana Chinnici\nTitolo: Conservazione preventiva dell
e collezioni del Museo: primi risultati del progetto SpecoLab\nAbstract: T
BD
DTSTART;TZID=Europe/Rome:20241023T150000
DTEND;TZID=Europe/Rome:20241023T163000
SEQUENCE:0
SUMMARY:Seminario: Ileana Chinnici (INAF)
URL:http://www.astropa.inaf.it/evento/seminario-ileana-chinnici-inaf-7/
X-COST-TYPE:free
X-ALT-DESC;FMTTYPE=text/html:\\n\\n\\n\\n\\nSpeaker: Ileana Chinnici
\nTitolo: Conservazio
ne preventiva delle collezioni del Museo: primi risultati del progetto Spe
coLab
\nAbstract: TBD
\n
END:VEVENT
END:VCALENDAR