Magnetic field variations in the Jovian magnetotail induced by solar wind dynamic pressure enhancements
Magnetic field variations in the Jovian magnetotail induced by solar wind dynamic pressure enhancements
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DOI：
10.1029/2004ja010959
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发表时间：
2005-11-11
影响因子：
2.8
通讯作者：
Yokoyama, T
中科院分区：
文献类型：
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作者：
Tao, C;Kataoka, R;Yokoyama, T
[1]为了了解木星磁层对太阳风动压增强的响应，我们研究了伽利略航天器观测到的磁场变化。通过模拟来自地球的太阳风的一维磁流体动力学（MHD）传播，克服了木星磁层上游缺乏太阳风监测的问题。我们识别出木星轨道上太阳风动压增加> 0.25 nPa的事件。特征磁场变化被发现在木星磁层的所有9个事件。由于木星旋转的矩形波形消失的九个事件中的八个。在频率范围从0.3到10 mHz的磁场扰动同时增强。扰动的最大振幅与太阳风动压的最大振幅成正比。我们认为，在压缩磁层下，电流片发生了很大的形变，并诱发了重联爆发。
[1] In order to understand the response of the Jovian magnetosphere to solar wind dynamic pressure enhancements, we investigate magnetic field variations observed by the Galileo spacecraft. The lack of solar wind monitoring just upstream of the Jovian magnetosphere is overcome by simulating a one-dimensional magnetohydrodynamic (MHD) propagation of the solar wind from the Earth. We identify the events with an increase of the solar wind dynamic pressure > 0.25 nPa at the Jovian orbit. Characteristic magnetic field variations are found in the Jovian magnetosphere for all of the nine events. The rectangular waveform due to the Jovian rotation disappears for eight of the nine events. Magnetic field disturbances in the frequency range from 0.3 to 10 mHz are enhanced simultaneously. The maximum amplitude of the disturbances is in proportional to the maximum amplitude of the solar wind dynamic pressure. We suggest that the current sheet is greatly deformed and reconnection bursts are induced under the compressed magnetosphere.