Tag: atmosfere

Photoevaporation in young planets. The study: “New Constraints on the Future Evaporation of the Young Exoplanets in the V1298 Tau System” of A. Maggio (INAF – OAPA) recently appeared on ApJ

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The search for young exoplanets is crucial to our understanding of the planetary formation process and the early evolution of planets. The disc of gas and dust from which planets form, in fact, typically disperse in a few million of years. Before that, the young planets interact with all the material orbiting around the star within the disk, triggering important

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Photospheric spots and planetary transits. The study: “Correcting the effect of stellar spots on ARIEL transmission spectra” of G. Cracchiolo (UNIPA, INAF-OAPA) appeared on MNRAS

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A “transit” occurs when we observe a planet moving across the disc of its star. Thus, during the transit the planet obscures a small portion of its star, slightly reducing its luminosity. While in the Solar System the only planets we can observe transiting in front of the Sun are Mercury and Venus, transits is still the most efficient method

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Thermal inversion in the atmosphere of a ultra-Hot Jupiter. The study: “Neutral Iron Emission Lines from the Dayside of KELT-9b: The GAPS Program with HARPS-N at TNG XX” of Pino L. (INAF/OA Arcetri; University of Amsterdam) recently appeared on ApJ

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Hot Jupiters are gaseous planets orbiting very close to their stars, typically closer than 0.1 Astronomical Units (the average distance between Earth and Sun), and with very short orbital periods of days or even hours. An extreme sub-class of these planets are the ultra-Hot Jupiters. These planets are tidally-locked to their stars (which means that they show always the same

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Artificial Intelligence applied to astrophysics. The paper “ExoGAN: Retrieving Exoplanetary Atmospheres Using Deep Convolutional Generative Adversarial Networks” of T. Zingales (UCL, INAF – OAPA) published on AJ

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In the last few years, many space missions and ground-based surveys, discovered more than 4000 exoplanets, especially using the transit and radial velocity methods. These two methods combined, give us a first estimation of the bulk density of the planets. In order to have a deeper understanding on the planetary characteristics and history, we also need to study their atmospheres.

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