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| Main Authors: | , , , , , |
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| Format: | Preprint |
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2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2403.17325 |
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| _version_ | 1866929288685551616 |
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| author | Yan, Dongdong Guo, Jianheng Seon, Kwang-il López-Puertas, Manuel Czesla, Stefan Lampón, Manuel |
| author_facet | Yan, Dongdong Guo, Jianheng Seon, Kwang-il López-Puertas, Manuel Czesla, Stefan Lampón, Manuel |
| contents | This paper presents a hydrodynamic simulation that couples detailed non-local thermodynamic equilibrium (NLTE) calculations of the hydrogen and helium level populations to model the H$α$ and He 10830 transmission spectra of the hot Jupiter HAT-P-32b. A Monte Carlo simulation is applied to calculate the number of Ly$α$ resonance scatterings, which is the main process for populating H(2). In the examined parameter space, only the models with H/He $\geq$ 99.5/0.5, $(0.5 \sim 3.0)$ times the fiducial value of $F_{\rm XUV}$, $β_m = 0.16\sim 0.3$, can explain the H$α$ and He 10830 lines simultaneously. We find a mass-loss rate of $\sim (1.0\sim 3.1) \times 10^{13}$ g s$^{-1}$, consistent with previous studies. Moreover, we find that the stellar Ly$α$ flux should be as high as $4 \times 10^{5}$ erg cm$^{-2}$ s$^{-1}$, indicating high stellar activity during the observation epoch of the two absorption lines. Despite the fact that the metallicity in the lower atmosphere of HAT-P-32b may be super-solar, our simulations tentatively suggest it is close to solar in the upper atmosphere. The difference in metallicity between the lower and upper atmospheres is essential for future atmospheric characterisations. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_17325 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | A possibly solar metallicity atmosphere escaping from HAT-P-32b revealed by H$α$ and He absorption Yan, Dongdong Guo, Jianheng Seon, Kwang-il López-Puertas, Manuel Czesla, Stefan Lampón, Manuel Earth and Planetary Astrophysics This paper presents a hydrodynamic simulation that couples detailed non-local thermodynamic equilibrium (NLTE) calculations of the hydrogen and helium level populations to model the H$α$ and He 10830 transmission spectra of the hot Jupiter HAT-P-32b. A Monte Carlo simulation is applied to calculate the number of Ly$α$ resonance scatterings, which is the main process for populating H(2). In the examined parameter space, only the models with H/He $\geq$ 99.5/0.5, $(0.5 \sim 3.0)$ times the fiducial value of $F_{\rm XUV}$, $β_m = 0.16\sim 0.3$, can explain the H$α$ and He 10830 lines simultaneously. We find a mass-loss rate of $\sim (1.0\sim 3.1) \times 10^{13}$ g s$^{-1}$, consistent with previous studies. Moreover, we find that the stellar Ly$α$ flux should be as high as $4 \times 10^{5}$ erg cm$^{-2}$ s$^{-1}$, indicating high stellar activity during the observation epoch of the two absorption lines. Despite the fact that the metallicity in the lower atmosphere of HAT-P-32b may be super-solar, our simulations tentatively suggest it is close to solar in the upper atmosphere. The difference in metallicity between the lower and upper atmospheres is essential for future atmospheric characterisations. |
| title | A possibly solar metallicity atmosphere escaping from HAT-P-32b revealed by H$α$ and He absorption |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2403.17325 |