SIMULATION OF THE H$\alpha$ ABSORPTION FOR THE HOT JUPITER HAT-P-32 B
Section: EXOPLANETS
Authors:
1.
Institute of Laser Physics, SB RAS
2.
Institute of Laser Physics, SB RAS
3.
Institute of Laser Physics, SB RAS
Institute of Astronomy of the Russian Academy of Sciences
Institute of Astronomy of the Russian Academy of Sciences
4.
Institute of Laser Physics, SB RAS
Institute of Astronomy of the Russian Academy of Sciences
Institute of Astronomy of the Russian Academy of Sciences
Type:
Сonference article
Published:
27.12.2024
Subject area:
52
53
520
521
523
524
52-1
52-6
41.00
29.35
29.31
29.33
29.27
29.05
03.06.01
03.05.01
03.04.03
2
223
614
6135
SCI004000
SCI005000
53
520
521
523
524
52-1
52-6
41.00
29.35
29.31
29.33
29.27
29.05
03.06.01
03.05.01
03.04.03
2
223
614
6135
SCI004000
SCI005000
Language:
English
Keywords:
planets and satellites: atmospheres; radiative transfer; scattering; hydrodynamics
Abstract (English):
The paper presents the results of modeling the absorption spectrum in the H$\alpha$ and He 10830 Å lines for the hot Jupiter HAT-P-32 b. The simulation was carried out using a 3D hydrodynamic model coupled to a Monte Carlo model of Ly$\alpha$ photon transfer. It was determined that to explain the absorption in both lines at a ratio ${\rm H}/{\rm He}=99/1$, high values of the XUV flux and stellar Ly$\alpha$ flux are required: $F_{\rm XUV}=100$ erg cm$^{-2}$ s$^{-1}$ and $I_{\rm Ly\alpha}=600$ erg cm$^{-2}$ s$^{-1}$, which may indicate high activity of the star. New parameters were also found that describe the absorption at ${\rm H}/{\rm He}=97/3$ while requiring less extreme $F_{\rm XUV}=25$ erg cm$^{-2}$ s$^{-1}$ and $I_{\rm Ly\alpha}=600$ erg cm$^{-2}$ s$^{-1}$. Monte Carlo modeling showed that the absorption in the H$\alpha$ line is formed by stellar photons producing H(2) concentrations at a level of $10^2$–$10^3$ cm$^{-3}$ in the atmospheric layer up to $2R_{\rm p}$, where the absorption occurs.
The paper presents the results of modeling the absorption spectrum in the H$\alpha$ and He 10830 Å lines for the hot Jupiter HAT-P-32 b. The simulation was carried out using a 3D hydrodynamic model coupled to a Monte Carlo model of Ly$\alpha$ photon transfer. It was determined that to explain the absorption in both lines at a ratio ${\rm H}/{\rm He}=99/1$, high values of the XUV flux and stellar Ly$\alpha$ flux are required: $F_{\rm XUV}=100$ erg cm$^{-2}$ s$^{-1}$ and $I_{\rm Ly\alpha}=600$ erg cm$^{-2}$ s$^{-1}$, which may indicate high activity of the star. New parameters were also found that describe the absorption at ${\rm H}/{\rm He}=97/3$ while requiring less extreme $F_{\rm XUV}=25$ erg cm$^{-2}$ s$^{-1}$ and $I_{\rm Ly\alpha}=600$ erg cm$^{-2}$ s$^{-1}$. Monte Carlo modeling showed that the absorption in the H$\alpha$ line is formed by stellar photons producing H(2) concentrations at a level of $10^2$–$10^3$ cm$^{-3}$ in the atmospheric layer up to $2R_{\rm p}$, where the absorption occurs.
Keywords:
planets and satellites: atmospheres; radiative transfer; scattering; hydrodynamics
planets and satellites: atmospheres; radiative transfer; scattering; hydrodynamics
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