The interaction between gas, stellar wind and energetic radiation in star forming regions: “The Gaia-ESO Survey: dynamics of ionized and neutral gas in the Lagoon nebula (M 8)” of F. Damiani published by A&A

Star forming regions are complex environments, shaped by the star formation process (which involves gravity, turbulence and magnetic fields) and the interaction between the clouds and the stellar winds and energetic radiation (X-ray and UV) produced by the newborn stars.   The interaction between clouds and stellar wind and radiation is of particular interest. Stellar radiation creates expanding fronts in

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The chemical evolution of our Galaxy studied with GES. The study: “The Gaia-ESO Survey: Galactic evolution of sulphur and zinc” of S. Duffau published on A&A

Stars more massive than 9 solar masses are efficient chemical labs, where hydrogen and helium are synthesized into other chemical elements, such as oxygen, carbon, and silicon. When these stars explode as supernovae (type I or “core-collpase” supernovae), these chemical elements are ejected into space, enriching the interstellar medium and being in future available to form new generations of stars.

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Supernovae and Jet, the letter: “Indications of a Si-rich bilateral jet of ejecta in the Vela SNR observed with XMM-Newton” by F. Garcia published on A&A

The life cycle of very massive stars ends in supernovae explosions. During these violent phenomena, an amount of energy similar to that produced by the Sun during its entire lifetime,more than 10 billion years long, is released in few seconds. Besides, the atmosphere of the exploding star (the progenitor star) is ejected with a velocity in excess of 1000 km/sec.

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Rotation of young stars studied in “Near-Infrared Time-Series Photometry in the Field of Cygnus OB2 Association” by J. Roquette (ICEx – UFMG)

Conservation of angular momentum is one of the fundamental laws of physic that every student must deal with. Let’s make an example: if we consider a rotating cloud of dust  and gas of our Galaxy and we let it collapse under its own gravity, and then form stars, the conservation of its angular momentum dictates a faster and faster rotation

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Published by F. Damiani (INAF-OAPA) on A&A the first extensive spectroscopic analysis of the stellar population of a massive star forming region (Carina Nebula)

Star forming regions form stars in associations or clusters as a consequence of the gravitational collapse of clouds. Typically, in the Milky Way star forming regions form hundreds to few thousands of stars. However, there exist also very massive star forming regions which form tens to hundreds of thousands stars, together with some of the most massive stars known in

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Published on A&A: “The Gaia-ESO Survey: radial distribution of abundances in the Galactic disc from open clusters and young-field stars” by L. Magrini

Massive stars are enormous chemical laboratories where heavy chemical elements are synthesized. For instance, the alpha-elements (O, Mg, Si, Ca, and Ti) are produced by nucleosynthetic processes in the interior of massive stars. Moreover, the lifetime of massive stars is much shorter than that of low mass stars: few million years for the former compared to several billion of years

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Pubblicato su MNRAS lo studio “Radio polarization maps of shell-type SNRs – II Sedov models with evolution of turbulent magnetic field” di O. Petruk

di Mario Giuseppe Guarcello    ( segui mguarce)     Le esplosioni di supernovae sono certamente tra i fenomeni più spettacolari che ci offre l’Universo. Questi fuochi d’artificio cosmici che segnano la morte di stelle molto massive rilasciano in pochi secondi l’energia irradiata dal Sole durante i suoi 10 miliardi di anni di esistenza. Gli strati esterni della stella vengono espulsi

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Pubblicato lo studio “The GAPS Programme with HARPS-N at TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets” di A. S. Bonomo (INAF-OATO)

di Mario Giuseppe Guarcello    ( segui mguarce)     A guardare il nostro Sistema Solare, sembrerebbe che il destino di un pianeta sia quello di girare attorno la sua stella in un’orbita stabile ed imperturbata. Ma se c’è una cosa che la ricerca sui pianeti extrasolari ci ha insegnato, è che non è affatto così.   Soprattutto nelle sue prime

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Pubblicato lo studio: “X-ray survey of the North-America and Pelican star-forming complex (NGC 7000/IC 5070)” di F. Damiani (INAF-OAPA)

di Mario Giuseppe Guarcello    ( segui mguarce)     Poche ma estremamente importanti…. Le stelle con masse maggiori di 6 masse solari ed una temperatura efficace maggiore di 15000 gradi (stelle O e stelle B1-B5) sono particolarmente rare nell’Universo e la loro evoluzione si compie in pochi milioni di anni, un tempo piuttosto breve se paragonato ai miliardi di anni

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Lo studio: “The GAPS Programme with HARPS-N at TNG. XV. A substellar companion around a K giant star identified with quasi-simultaneous HARPS-N and GIANO measurements” di E. González-Álvarez accettato per essere pubblicato su A&A

di Mario Giuseppe Guarcello    ( segui mguarce)     Il Sistema Solare non rimarrà così in eterno. Tra circa cinque miliardi di anni, quando non potrà più produrre energia bruciando idrogeno, il nostro Sole evolverà dalla fase di sequenza principale alla fase di gigante rossa, aumentando le proprie dimensioni a discapito dei pianeti più vicini ad esso.   Chiaramente è

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