MAGNETIC DRAG ON HOT JUPITER ATMOSPHERIC WINDS

被引：144
|
作者：
Perna, Rosalba [1 ,2 ]
Menou, Kristen [3 ,4 ]
Rauscher, Emily [3 ,4 ]
机构：
[1] Univ Colorado, JILA, Boulder, CO 80309 USA
[2] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA
[3] Columbia Univ, Dept Astron, New York, NY 10027 USA
[4] UCSB, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA
来源：
ASTROPHYSICAL JOURNAL | 2010年 / 719卷 / 02期
基金：
美国国家科学基金会;
关键词：
planets and satellites: atmospheres; planets and satellites: individual (HD 209458b); planets and satellites: magnetic fields; GENERAL-CIRCULATION; SIMULATIONS; DYNAMICS; MODEL;
D O I：
10.1088/0004-637X/719/2/1421
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Hot Jupiters, with atmospheric temperatures T greater than or similar to 1000 K, have residual thermal ionization levels sufficient for the interaction of ions with the planetary magnetic field to result in a sizable magnetic drag on the (neutral) atmospheric winds. We evaluate the magnitude of magnetic drag in a representative three-dimensional atmospheric model of the hot Jupiter HD 209458b and find that it is a plausible mechanism to limit wind speeds in this class of atmospheres. Magnetic drag has a strong geometrical dependence, both meridionally and from the dayside to the nightside (in the upper atmosphere), which could have interesting consequences for the atmospheric flow pattern. By extension, close-in eccentric planets with transiently heated atmospheres will experience time-variable levels of magnetic drag. A robust treatment of magnetic drag in circulation models for hot atmospheres may require iterated solutions to the magnetic induction and Saha equations as the hydrodynamic flow is evolved.
引用
收藏
页码：1421 / 1426
页数：6
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