Simulations of radiation belt formation during storm sudden commencements
Simulations of radiation belt formation during storm sudden commencements
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DOI：
10.1029/97ja03995
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发表时间：
1997-01
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影响因子：
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通讯作者：
M. Hudson;S. Elkington;J. Lyon;V. A. Marchenko;I. Roth;M. Temerin;J. Blake;M. Gussenhoven;J. Wygant
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文献类型：
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作者：
M. Hudson;S. Elkington;J. Lyon;V. A. Marchenko;I. Roth;M. Temerin;J. Blake;M. Gussenhoven;J. Wygant
来自1991年3月24日大风暴突然开始（SSC）的全球三维模拟的MHD场用于跟踪该事件期间辐射带形成的引导中心测试粒子模拟中的粒子轨迹。建模不太激烈的事件在CRRES卫星的寿命，具有类似的形态，但较少的径向运输和辐射，也提出了。在所有的情况下分析，一个太阳质子事件后，SSC，导致形成一个新的质子带地球太阳质子渗透。研究了太阳风和模式脉冲参数变化对粒子运动的影响。太阳质子的种子种群和SSC冲击引起的磁层压缩都是形成新质子带的必要条件。内区质子的外边界可能受到SSC的影响，新形成的带可能受到随后或随后的风暴的影响，这些风暴可能会迅速连续发生，就像1991年6月和7月的情况一样。加速过程是有效的向北和向南的IMF，与更多的向南的情况下，否则可比的太阳风参数，因为最初更多的压缩磁层顶在向南的情况下，与更多的径向和向内的径向运输。新形成的带的内边界和稳定性取决于形成时的径向输运的大小和随后的绝热俘获环电流扰动。
MHD fields from a global three‐dimensional simulation of the great March 24, 1991, storm sudden commencement (SSC) are used to follow the trajectories of particles in a guiding center test particle simulation of radiation belt formation during this event. Modeling of less intense events during the lifetime of the CRRES satellite, with similar morphology but less radial transport and energization, is also presented. In all cases analyzed, a solar proton event was followed by an SSC, leading to the formation of a new proton belt earthward of solar proton penetration. The effect on particle energization of varying solar wind and model pulse parameters is investigated. Both a seed population of solar protons and the SSC shock‐induced compression of the magnetosphere are necessary conditions for the formation of a new proton belt. The outer boundary of the inner zone protons can be affected by an SSC and a newly formed belt can be affected by the ensuing or a subsequent storm, which may occur in rapid succession, as was the case in June and July 1991. The acceleration process is effective for both northward and southward IMF, with more energization and inward radial transport for the southward case for otherwise comparable solar wind parameters, because of the initially more compressed magnetopause in the southward case. The inner boundary and stability of the newly formed belt depends on the magnitude of radial transport at the time of formation and subsequent ring current perturbation of adiabatic trapping.