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MESSENGER Observations of Extreme Loading and Unloading of Mercury's Magnetic Tail

机译：MESSENGER观察水星磁尾的极端装卸

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摘要

During MESSENGER'S third flyby of Mercury, the magnetic field in the planet's magnetic tail increased by factors of 2 to 3.5 over intervals of 2 to 3 minutes. Magnetospheric substorms at Earth are powered by similar tail loading, but the amplitude is lower by a factor of ～10 and typical durations are ～1 hour. The extreme tail loading observed at Mercury implies that the relative intensity of substorms must be much larger than at Earth. The correspondence between the duration of tail field enhancements and the characteristic time for the Dungey cycle, which describes plasma circulation through Mercury's magnetosphere, suggests that such circulation determines the substorm time scale. A key aspect of tail unloading during terrestrial substorms is the acceleration of energetic charged particles, but no acceleration signatures were seen during the MESSENGER flyby.
机译：在MESSENGER的第三次水星飞越期间，行星磁尾中的磁场在2到3分钟的间隔内增加了2到3.5倍。地球上的磁层副风暴由相似的尾部载荷驱动，但振幅降低了约10倍，典型持续时间约为1小时。在水星上观察到的极端尾部载荷意味着亚暴的相对强度必须比在地球上大得多。尾场增强的持续时间与Dungey循环的特征时间之间的对应关系描述了通过水星磁层的等离子体循环，表明这种循环决定了亚暴的时间尺度。地面亚暴期间尾翼卸载的一个关键方面是高能带电粒子的加速，但是在MESSENGER飞越过程中没有看到加速信号。

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  • 来源
    《Science》 |2010年第5992期|P.665-668|共4页
  • 作者

    James A. Slavin; Brian J. Anderson; Daniel N. Baker; Mehdi Benna; Scott A. Boardsen; George Gloeckler; Robert E. Gold; George C. Ho; Haje Korth; Stamatios M. Krimigis; Ralph L. McNutt Jr.; Larry R. Nittler; Jim M. Raines; Menelaos Sarantos; David Schriver; Sean C. Solomon; Richard D. Starr; Pavel M. Travnicek; Thomas H. Zurbuchen;

  • 作者单位

    Heliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA;

    rnJohns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA;

    Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA Department of Physics and Astrophysical and Planetary Sciences Department, University of Colorado, Boulder, CO 80303, USA;

    rnSolar System Exploration Division, NASA Goddard Space Flight Center,Greenbelt, MD 20771, USA Goddard Earth Science and Technology Center, University of Maryland, Baltimore County,Baltimore, MD 21228, USA;

    rnHeliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Goddard Earth Science and Technology Center, University of Maryland, Baltimore County,Baltimore, MD 21228, USA;

    rnDepartment of Astronomy, University of Maryland, College Park, MD 20742, USA Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, MI 48109, USA;

    rnJohns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA;

    rnJohns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA;

    rnJohns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA;

    rnJohns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA Academy of Athens,Athens 11527, Greece;

    rnJohns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA;

    rnDepartment of Terrestrial Magnetism,Carnegie Institution of Washington, Washington, DC 20015, USA;

    rnDepartment of Astronomy, University of Maryland, College Park, MD 20742, USA;

    rnHeliophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Goddard Earth Science and Technology Center, University of Maryland, Baltimore County,Baltimore, MD 21228, USA;

    rnInstitute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90024, USA;

    rnDepartment of Terrestrial Magnetism,Carnegie Institution of Washington, Washington, DC 20015, USA;

    rnDepartment of Physics, Catholic University of America, Washington, DC 20064,USA;

    rnInstitute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90024, USA Astronomical Institute, Academy of Sciences of the Czech Republic, Prague 14131, Czech Republic;

    rnDepartment of Astronomy, University of Maryland, College Park, MD 20742, USA;

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