On the star-magnetosphere interaction of close-in exoplanets

Wing Huen Ip; Andreas Kopp; Juei Hwa Hu

doi:10.1086/382274

On the star-magnetosphere interaction of close-in exoplanets

Wing Huen Ip, Andreas Kopp, Juei Hwa Hu

Graduate Institute of Astronomy

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Abstract

Numerical simulations using a resistive MHD code are performed in order to investigate the interaction of the magnetospheres of hot Jupiters (or close-in extrasolar giant planets) with the central host stars. Because of the sub-Alfvénic nature of the stellar wind outflow at the orbital positions of these close-in exoplanets, no bow shock would form. When the orientation of the stellar coronal magnetic field is favorable to strong coupling with magnetic reconnection, the power (∼10²⁷ ergs s^-1) generated could reach the level of a typical solar flare. As a particular type of star-planet atmospheric interaction, as investigated by Cuntz, Saar, & Musielak, magnetospheric interaction as studied in this Letter could lead to extensive energy injection into the auroral zones of the exoplanets, producing massive atmospheric escape process as recently detected.

Original language	English
Pages (from-to)	L53-L56
Journal	Astrophysical Journal
Volume	602
Issue number	1 II
DOIs	https://doi.org/10.1086/382274
State	Published - 10 Feb 2004

Keywords

Magnetic fields
Planetary systems
Stars: atmospheres
Stars: chromospheres
Stars: flare

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10.1086/382274

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title = "On the star-magnetosphere interaction of close-in exoplanets",

abstract = "Numerical simulations using a resistive MHD code are performed in order to investigate the interaction of the magnetospheres of hot Jupiters (or close-in extrasolar giant planets) with the central host stars. Because of the sub-Alfv{\'e}nic nature of the stellar wind outflow at the orbital positions of these close-in exoplanets, no bow shock would form. When the orientation of the stellar coronal magnetic field is favorable to strong coupling with magnetic reconnection, the power (∼1027 ergs s-1) generated could reach the level of a typical solar flare. As a particular type of star-planet atmospheric interaction, as investigated by Cuntz, Saar, & Musielak, magnetospheric interaction as studied in this Letter could lead to extensive energy injection into the auroral zones of the exoplanets, producing massive atmospheric escape process as recently detected.",

keywords = "Magnetic fields, Planetary systems, Stars: atmospheres, Stars: chromospheres, Stars: flare",

author = "Ip, {Wing Huen} and Andreas Kopp and Hu, {Juei Hwa}",

note = "Funding Information: The authors would like to thank Steve Miller and Tom Kri-migis for useful discussions. We also thank Hsiang-Wen Hsu for providing Figure 3. The careful review and constructive comments by the reviewer are very much appreciated. This work was partly supported by NSC 92-2112-M-008-023 and NSC 92-2111-M-008-001, Taiwan and by the Ministry of Education of Taiwan through the CosPA Project 92-N-FA01-1-4-5.",

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AU - Ip, Wing Huen

AU - Kopp, Andreas

AU - Hu, Juei Hwa

N1 - Funding Information: The authors would like to thank Steve Miller and Tom Kri-migis for useful discussions. We also thank Hsiang-Wen Hsu for providing Figure 3. The careful review and constructive comments by the reviewer are very much appreciated. This work was partly supported by NSC 92-2112-M-008-023 and NSC 92-2111-M-008-001, Taiwan and by the Ministry of Education of Taiwan through the CosPA Project 92-N-FA01-1-4-5.

PY - 2004/2/10

Y1 - 2004/2/10

N2 - Numerical simulations using a resistive MHD code are performed in order to investigate the interaction of the magnetospheres of hot Jupiters (or close-in extrasolar giant planets) with the central host stars. Because of the sub-Alfvénic nature of the stellar wind outflow at the orbital positions of these close-in exoplanets, no bow shock would form. When the orientation of the stellar coronal magnetic field is favorable to strong coupling with magnetic reconnection, the power (∼1027 ergs s-1) generated could reach the level of a typical solar flare. As a particular type of star-planet atmospheric interaction, as investigated by Cuntz, Saar, & Musielak, magnetospheric interaction as studied in this Letter could lead to extensive energy injection into the auroral zones of the exoplanets, producing massive atmospheric escape process as recently detected.

AB - Numerical simulations using a resistive MHD code are performed in order to investigate the interaction of the magnetospheres of hot Jupiters (or close-in extrasolar giant planets) with the central host stars. Because of the sub-Alfvénic nature of the stellar wind outflow at the orbital positions of these close-in exoplanets, no bow shock would form. When the orientation of the stellar coronal magnetic field is favorable to strong coupling with magnetic reconnection, the power (∼1027 ergs s-1) generated could reach the level of a typical solar flare. As a particular type of star-planet atmospheric interaction, as investigated by Cuntz, Saar, & Musielak, magnetospheric interaction as studied in this Letter could lead to extensive energy injection into the auroral zones of the exoplanets, producing massive atmospheric escape process as recently detected.

KW - Magnetic fields

KW - Planetary systems

KW - Stars: atmospheres

KW - Stars: chromospheres

KW - Stars: flare

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DO - 10.1086/382274

M3 - 期刊論文

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SN - 0004-637X

VL - 602

SP - L53-L56

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 II

ER -

On the star-magnetosphere interaction of close-in exoplanets

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Keywords

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