Shedding lights on the mechanism responsible for the formation of Hot Jupiters. The study: “Gas, not dust: Migration of TESS/Gaia hot Jupiters possibly halted by the magnetospheres of protoplanetary disks” of I. Mendigutia (CAB) appeared on A&A

Hot Jupiters are gas giants that orbit at distances less than 0.1 AU from their host star. But what determines the final orbital radius of these planets? In intermediate-mass stars, it seems to be the dispersion of gas in their protoplanetary disks.   Hot Jupiters are a class of exoplanets that are not found in our Solar System. They are

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The program “Testing protoplanetary disk evolution and brown dwarf formation in starburst: NIRCAM and MIRI observations of the young cluster Westerlund 1” of M. G. Guarcello (INAF – OAPA) is among the accepted proposals of the JWST Cycle 1

The James Webb Telescope (JWST) will be the most complex and powerful telescope ever launched into space. Built by a consortium formed by NASA, ESA, and the Canadian Space Agency (CSA), thanks to its primary mirror with a diameter of 6.5 meters (for comparison, the mirror of the Hubble Space Telescope has a diameter of 2.5 meters) and its four

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MHD simulations of the radio emission from a flaring T Tauri star. The study: “Predicting the time variation of radio emission from MHD simulations of a flaring T-Tauri star” of Waterfall C. O. G. (Jodrell Bank Centre for Astrophysics) recently appeared on MNRAS

T Tauri stars are young low-mass stars (typically younger than 5 million of years), which are surrounded by a protoplanetary disk, e.g. a disk of gas and dust orbiting around the star. The disk material does not reach the central star: the dust component sublimates in the inner disk, where the temperature exceeds 1500 degrees, while the gas disk is truncated

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Accretion and dispersion of protoplanetary disks. The study: “X-shooter spectroscopy of young stars with disks. The TW Hydrae association as a probe of the final stages of disk accretion” by L. Venuti (Eberhard Karls Universität/Cornell University/NASA) recently published by A&A

At a distance of about 160 light years, the stellar association TW Hydrae is a benchmark for the study of pre-main sequence stars and their protoplanetary disks. Pre-main sequence stars are a few million years old stars, still gravitationally contracting and not powered yet by the thermonuclear reactions. They are often surrounded by disks of dust and gas called “protoplanetary

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Accretion funnels connecting the young stars in Orion and their protoplanetary disks. The study “X-Ray Flare Oscillations Track Plasma Sloshing along Star-disk Magnetic Tubes in the Orion Star-forming Region” of F. Reale published on ApJ

di Mario Giuseppe Guarcello    ( segui mguarce)     A recent study by a team of researchers of INAF-Astronomical Observatory of Palermo, the University of Palermo, and the University of Madrid, recently published on the Astrophysical Journal, shows that  enormous flares in the young stars in Orion are due to large magnetic loops connecting the stars and their protoplanetary disks,

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