Simulation of proton radiation belt formation during the March 24, 1991 SSC
Simulation of proton radiation belt formation during the March 24, 1991 SSC
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DOI：
10.1029/95gl00009
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发表时间：
1995-02
影响因子：
5.2
通讯作者：
M. Hudson;A. D. Kotelnikov;Xinlin Li;I. Roth;M. Temerin;J. Wygant;J. Blake;M. Gussenhoven
中科院分区：
文献类型：
--
作者：
M. Hudson;A. D. Kotelnikov;Xinlin Li;I. Roth;M. Temerin;J. Wygant;J. Blake;M. Gussenhoven
利用相对论导向中心试验粒子程序模拟了1991年3月24日CRRES卫星观测到的风暴突发事件（SSC）后，在L_2.5处迅速形成的新质子辐射带。SSC由双极电场和叠加在偶极磁场上的磁场中的相关压缩和弛豫来建模。源人口由太阳和捕获的内区质子。模拟结果表明，虽然这两个人口有助于漂移回波在20-80兆电子伏的范围内，主要的贡献是从太阳质子。SSC对质子的加速不同于相对论电子加速，因为不同的源粒子数对加速有贡献，并且第一绝热不变量的非相对论守恒导致对于给定的L减小，质子的相对论性更大。模型漂移回波和通量分布在L在注射时比较以及与CRRES观测。
The rapid formation of a new proton radiation belt at L ≃ 2.5 following the March 24, 1991 Storm Sudden Commencement (SSC) observed at the CRRES satellite is modelled using a relativistic guiding center test particle code. The SSC is modelled by a bipolar electric field and associated compression and relaxation in the magnetic field, superimposed on a dipole magnetic field. The source population consists of both solar and trapped inner zone protons. The simulations show that while both populations contribute to drift echoes in the 20–80 MeV range, primary contribution is from the solar protons. Proton acceleration by the SSC differs from relativistic electron acceleration in that different source populations contribute and nonrelativistic conservation of the first adiabatic invariant leads to greater energization of protons for a given decrease in L. Model drift echoes and flux distribution in L at the time of injection compare well with CRRES observations.