Simulating the Escaping Atmosphere of GJ 436 b with Two-fluid Magnetohydrodynamic Models

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外文摘要：Observations of transmission spectra reveal that hot Jupiters and Neptunes are likely to possess escaping atmospheres driven by stellar radiation.Numerous models predict that magnetic fields may exert significant influences on the atmospheres of hot planets.Generally,the escaping atmospheres are not entirely ionized,and magnetic fields only directly affect the escape of ionized components within them.Considering the chemical reactions between ionized components and neutral atoms,as well as collision processes,magnetic fields indirectly impact the escape of neutral atoms,thereby influencing the detection signals of planetary atmospheres in transmission spectra.In order to simulate this process,we developed a magnetohydrodynamic multi-fluid model based on MHD code PLUTO.As an initial exploration,we investigated the impact of magnetic fields on the decoupling of H+and H in the escaping atmosphere of the hot Neptune GJ436b.Due to the strong resonant interactions between H and H+,the coupling between them is tight even if the magnetic field is strong.Of course,alternatively,our work also suggests that merging H and H+into a single flow can be a reasonable assumption in MHD simulations of escaping atmospheres.However,our simulation results indicate that under the influence of magnetic fields,there are noticeable regional differences in the decoupling of H+and H.With the increase of magnetic field strength,the degree of decoupling also increases.For heavier particles such as O,the decoupling between O and H+is more pronounced.Our findings provide important insights for future studies on the decoupling processes of heavy atoms in the escaping atmospheres of hot Jupiters and hot Neptunes under the influence of magnetic fields.

外文关键词：

magnetohydrodynamics(MHD)planets and satellites:atmosphereshydrodynamics

作者：

Lei Xing、Jianheng Guo、Chuyuan Yang、Dongdong Yan

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作者单位：

Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China

University of Chinese Academy of Sciences,Beijing 100049,China

Key Laboratory for Structure and Evolution of Celestial Objects,Chinese Academy of Sciences,Kunming 650216,China

International Centre of Supernovae,Yunnan Key Laboratory,Kunming 650216,China

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基金：

Strategic Priority Research Program of Chinese Academy of SciencesNational Natural Science Foundation of China(NSFC)National Natural Science Foundation of China(NSFC)National Natural Science Foundation of China(NSFC)National Natural Science Foundation of China(NSFC)National Natural Science Foundation of China(NSFC)National Key R&D Program of ChinaNatural Science Foundation of Yunnan ProvinceInternational Centre of Supernovae,Yunnan Key Laboratory

项目编号：

XDB 41000000122881021197308242305136U2031111122330062021YFA1600400/2021YFA1600402202201AT070158202302AN360001

出版年：

2024

DOI：

10.1088/1674-4527/ad47de

天文和天体物理学研究

中国科学院国家天文台

天文和天体物理学研究

CSTPCD

影响因子：0.406

ISSN：1674-4527

年,卷(期)：2024.24(6)