Electron heating in superhigh mach number shocks
Electron heating in superhigh mach number shocks
复制标题
超高马赫数冲击中的电子加热
DOI：
10.1007/978-94-009-3021-6_36
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发表时间：
1988
影响因子：
1.9
通讯作者：
K. Papadopoulos
中科院分区：
文献类型：
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作者：
K. Papadopoulos
流体和磁流体模型，以及在高马赫数范围(3≤MF≤12)到超高马赫数范围(Mf>；30-40)的地球弓激波测量的直接外推预测，下游电子压力只是朗肯-胡格尼奥特下游压力2的一小部分，即Pe_2/p_2≈Mf_2)−_1。然而，解释由于超新星激波加热而产生的X射线超新星发射需要2/p_2≈_0(1)。在Alfvén之后，我们使用等离子体物理实验理论数据结合磁层观测来探索SHMN激波的物理。如下所示，在反射和传输的离子与激波“脚下”的电子的相互作用中包含了适当的等离子体物理考虑，导致了令人惊讶的结果，即电子加热可以在SHNM范围内占主导地位。导出了激波结构的定常模型，并证明它是高马赫数激波物理外推的结果，并在底部加入了集体相互作用。
Fluid and MHD models, as well as direct extrapolation of the Earth’s bow shock measurements in the high Mach number (HMN) range (3 ≤MF≤ 12) to the superhigh Mach number (SHMN) range (MF> 30–40) predict that the downstream electron pressurepe2is only a negligible fraction of the Rankine-Hugoniot downstream pressurep2, i.e.,Pe2/p2≈MF2)−1. However, the interpretation of X-ray supernovae emissions, due to SHMN shock heating requirespe2/p2≈ 0(1). Following Alfvén we have used plasma physics experimental-theoretical data combined with magnetospheric observations to probe the physics of the SHMN shocks. It is shown below that inclusion of proper plasma physics considerations in the interaction of the reflected and transmitted ions and the electrons at the ‘foot’ of the shock leads to the surprising result that electron heating can dominate in the SHNM range. A stationary model of the shock structure is derived and shown to be the result of extrapolation of the high Mach number shock physics with incorporation of collective interactions at the foot.