Numerical simulation of flare‐generated disturbances in the solar wind
Numerical simulation of flare‐generated disturbances in the solar wind
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太阳风中耀斑产生的扰动的数值模拟
DOI：
10.1029/ja074i011p02908
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发表时间：
1969
期刊：
影响因子：
--
通讯作者：
R. Gentry
中科院分区：
文献类型：
--
作者：
A. Hundhausen;R. Gentry
利用含时流体动力学方程的数值解研究了耀斑产生的激波在太阳风中的传播。这些解对所有激波强度都是有效的，包括在太阳风中观测到的中间值，并考虑到环境太阳风特性的变化。能量沉积在扰动的时间尺度的整个范围内，从脉冲（产生“爆炸波”）连续沉积，被认为是。对于前一类扰动，其解接近极限形式，仅依赖于波的总能量。在爆炸波极限下，发现了能量、1 Au处的冲击强度和到1 Au的渡越时间之间的关系。对于能量在1031尔格附近的扰动，波从太阳传播到1 Au需要1060小时，在后一个距离处，波的传播之前有一个中等强度的激波。渡越时间和冲击强度都与直接观测值符合得很好。
The propagation of flare-generated shock waves through the solar wind is examined using numerical solutions of the time-dependent hydrodynamic equations. These solutions are valid for all shock strengths, including the intermediate values that have been observed in the solar wind, and take into account the variation of the properties of the ambient solar wind. The entire range of time scales for energy deposition in the disturbance, from impulsive (producing ‘blast waves’) to continuous deposition, is considered. For the former class of disturbances the solutions approach a limiting form dependent only on the total energy in the wave. Relationships among the energy, shock strength at 1 AU, and transit time to 1 AU are found in the blast wave limit. For disturbances with energies near 1031 ergs, the wave propagates from the sun to 1 AU in ∼60 hours, and is preceded by an intermediate strength shock at the latter distance. Both the transit time and shock strength are in good agreement with directly observed values.