Modeling of Absorption in the Hα Line for the Exoplanet WASP-52b

S. S. Sharipov; Шарипов С. С.; I. B. Miroshnichenko; Мирошниченко И. Б.; I. F. Shaikhislamov; Шайхисламов И. Ф.

doi:10.31857/S0004629923030076

Modeling of Absorption in the Hα Line for the Exoplanet WASP-52b

Authors: Sharipov S.S.¹^,2, Miroshnichenko I.B.¹^,2, Shaikhislamov I.F.¹
Affiliations:
1. Institute of Laser Physics, Siberian Branch, Russian Academy of Sciences
2. Novosibirsk State Technical University
Issue: Vol 100, No 3 (2023)
Pages: 281-288
Section: Articles
URL: https://journals.rcsi.science/0004-6299/article/view/139073
DOI: https://doi.org/10.31857/S0004629923030076
EDN: https://elibrary.ru/PODJEB
ID: 139073

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Abstract
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Abstract

The results of modeling the Hα absorption spectrum of the atmosphere of the hot Jupiter WASP‑52b are presented. The atmosphere was modeled with a three-dimensional hydrodynamic code. Several different values of the XUV ionizing radiation were considered. The Lyα-photon transfer in the atmosphere was simulated by the Monte Carlo method. Spatial distributions of the volume density of hydrogen atoms excited to the second energy level H(2) were obtained, and absorption spectra in the Hα line were calculated. It was also shown that absorption takes place in a layer with a thickness of about 1.5 times the planetary radius, while the greatest influence on absorption is exerted by Lyα photons produced due to recombination of electrons and protons.

Keywords

exoplanets, atmosphere, Monte Carlo, resonance scattering, transit observations, numerical modeling

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