The atmosphere of escaping hydrogen and helium from an exoplanet has been studied using advanced simulations

تمت دراسة الغلاف الجوي للهروب من الهيدروجين والهيليوم من كوكب خارج المجموعة الشمسية باستخدام عمليات محاكاة متقدمة (2022). DOI: 10.3847 / 1538-4357 / ac8793″ width=”800″ height=”322″/>

Astral XUV and FUV/NUV SED, the ε Eri spectrum taken from the MUSCLES Treasury Survey (France et al. 2016) and measured over the orbital distance of WASP-52b. In panel (a), the different solid lines represent the composite spectra of different micrometers. βm = 0.22 corresponds to the reference spectrum taken from the MUSCLES cabinet survey. attributed to him: Astrophysical Journal (2022). DOI: 10.3847 / 1538-4357 / ac8793

Researchers from the Yunnan Observatories of the Chinese Academy of Sciences and their collaborators reproduce the observed transmission spectra of exoplanet WASP-52b at different wavelength ranges and study the properties of atmospheric hydrogen and helium.

The results have been published in Astrophysical Journal On the 13th of September.

Exoplanets close to the Solar System receive high-energy radiation from their host stars, such as X-rays and extreme ultraviolet (XUV) radiation. In gas-rich exoplanets, this high-energy radiation may be absorbed by the atmosphere, thus heating the atmosphere and causing it to expand to overcome the gravitational potential of the planet and escape into the interstellar medium.

This phenomenon is known as planetary atmospheric escape, which can cause a significant amount of material to be lost from the planet and has important effects on planet formation, evolution, and even the general distribution of the planet.

The composition and properties of the planetary atmosphere can be studied by analyzing the absorption of spectral lines in different wavelength ranges, for example, optical band lines (Hα) and near infrared band (He λ10830Å), the so-called lines transition spectra.

In this study, the researchers used a hydrodynamic atmospheric escape model and a radiation transmission model to simulate the transmission spectra of WASP-52b. They presented a Monte Carlo model to simulate Lyα resonance scattering within the atmospheres of exoplanets for the first time, assuming that both the stellar Lyα radiation and the planetary atmosphere are in a spheroid.

Based on the distribution of the Lyα Pα dispersion rate, the researchers calculated the uptake of Hα, which is caused by hydrogen atoms In the first excited states. They also calculated the distribution of the transported helium atoms in detail and simulated the transmission spectra for hot Jupiter WASP-52b in the optical (Hα) and near-infrared (He λ10830Å) bands.

They have restricted the level of X-rays and intense UV rays radiation Received by the planet, as well as the ratio of the abundance of hydrogen to helium in the planetary atmosphere, revealing hydrogen And helium originated from the fugitive atmosphere. The results can help constrain the physical parameters of ambiance And to better understand its composition and structure.

Signals in the optical range can be used as a probe to detect escape from the atmosphere of hot Jupiters

more information:
Dongdong Yan et al, Modeling the Hα and He 10830 transmission spectrum of WASP-52b, Astrophysical Journal (2022). DOI: 10.3847 / 1538-4357 / ac8793

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