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arXiv 0706.0922physics.space-phphysics.geo-ph
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地磁风暴期间用低空卫星资料研究magnetosphere内部等离子体压力的径向分布：1982年3月1-8日事件

Radial distribution of the inner magnetosphere plasma pressure using low-altitude satellite data during geomagnetic storm: the March 1-8, 1982 Event

M. Stepanova, E. E. Antonova, J. M. Bosqued

备注：
Accepted in Advances in Space Research
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摘要：

内磁层等离子体压力分布是了解磁暴和亚磁暴等磁层主要过程的关键参数之一。然而，通过高空卫星现场粒子测量获得的压力分布不允许跟踪与风暴和亚暴有关的压力变化，因为这样做所需的时间间隔通常超过了它们的特征时间。相反，低空卫星的快速运动使得有可能利用沉降粒子的通量来反演沿卫星轨道的等离子体压力的准瞬时分布。在这项研究中，我们使用Aureol-3卫星数据等离子体压力估计，和IGRF，Tsyganenko 2001年和Tsyganenko 2004年风暴时间地磁场模型的压力映射到赤道平面。结果发现，在平静的地磁条件下，径向压力分布得到的轮廓，以前从高空测量得到的一致。相反，在磁暴期间，等离子体压力剖面变得更加尖锐，等离子体压力最大值的位置与Dst最小值对应，磁层内静压力最大值与太阳风动压力相关。等离子体压力廓线的增加表明，交换不稳定性可能是磁暴主相发展的重要因素之一。

英文摘要：

Plasma pressure distribution in the inner magnetosphere is one of the key parameters for understanding the main magnetospheric processes including geomagnetic storms and substorms. However, the pressure profiles obtained from in-situ particle measurements by the high-altitude satellites do not allow tracking the pressure variations related to the storms and substorms, because a time interval needed to do this generally exceeds the characteristic times of them. On contrary, fast movement of low-altitude satellites makes it possible to retrieve quasi-instantaneous profiles of plasma pressure along the satellite trajectory, using the fluxes of precipitating particles. For this study, we used the Aureol-3 satellite data for plasma pressure estimation, and the IGRF, Tsyganenko 2001 and Tsyganenko 2004 storm time geomagnetic field models for the pressure mapping into the equatorial plane. It was found that during quiet geomagnetic condition the radial pressure profiles obtained coincide with the profiles, obtained previously from the high-altitude measurements. On the contrary, it was found that during geomagnetic storm the plasma pressure profiles became sharper; the position of the maximum of plasma pressure corresponds to expected one for given Dst minimum; the maximum value of inner magnetosphere static pressure correlates with the solar wind dynamic pressure. Increase in the plasma pressure profiles indicates the possibility to consider the interchange instability as one of important factors for the development of the main phase of geomagnetic storm.

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