摘要
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.
原文 | ???core.languages.en_GB??? |
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頁(從 - 到) | L53-L56 |
期刊 | Astrophysical Journal |
卷 | 602 |
發行號 | 1 II |
DOIs | |
出版狀態 | 已出版 - 10 2月 2004 |