Stably trapped proton limits for Jupiter
Stably trapped proton limits for Jupiter
复制标题
木星稳定捕获的质子极限
DOI：
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发表时间：
1972
期刊：
影响因子：
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通讯作者：
C. Kennel
中科院分区：
文献类型：
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作者：
C. Kennel
本文介绍了地球和木星磁层的俯仰角扩散。在地球磁层中可能限制俘获通量的不稳定性被确定为交换或气球模、静电损失锥模和电磁离子回旋波。讨论了离子回旋波的不稳定性理论。只有当质子与波发生回旋共振时，这种波才是不稳定的。不稳定性增长率与回旋频率、快粒子分数密度和快粒子分布的各向异性成正比。临界质子能量是稳定捕获极限适用的最低能量，并且在L = 2和10个离子对/cu cm时计算为150 MeV。考虑临界阈值能量以上的粒子，其稳定性极限约为3 × 10的10次方/平方厘米/秒除以L的4次方。
A general introduction to pitch-angle diffusion for Earth and Jupiter magnetospheres is given. The instabilities which might limit the trapped fluxes in the earth magnetosphere are identified as the interchange or ballooning mode, electrostatic loss cone modes, and electromagnetic ion cyclotron wave. The instability theory of the ion cyclotron wave is discussed. This wave can be unstable only if protons can be in cyclotron resonance with the wave. The instability growth rate is proportional to the cyclotron frequency, the fractional number density of fast particles, and the anisotropy of the fast particle distribution. The critical proton energy is the lowest energy for which the stably trapped limit applies, and is calculated to be 150 MeV at L = 2 and for 10 ion pairs/cu cm. Particles above the critical threshold energy are considered and their stability limit is approximately 3 x 10 to the 10th power/sq cm/sec divided by L to the 4th power.