Electron energy flux in the solar wind
Electron energy flux in the solar wind
复制标题
太阳风中的电子能量通量
DOI：
10.1029/ja076i034p08165
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发表时间：
1971
期刊：
影响因子：
--
通讯作者：
M. Sugiura
中科院分区：
文献类型：
--
作者：
K. Ogilvie;J. Scudder;M. Sugiura
本文描述了太阳风中10 eV到9.9keV之间的电子的研究。对等离子体静止坐标系中的能量传输进行了评估，结果表明它与行星际磁场是平行的。来自太阳事件的电子的存在导致这个能量流密度E∥超过热流H∥，这是由于热电子。在一个这样的事件中，观测到的结果与在更高能量下进行的太阳电子观测是一致的。当在通过行星际场线与地球弓激波相连的点上进行观测时，可以观察到较大的能量通量沿场向太阳，但在此时间间隔内H∥保持向外定向。在任何一种情况下，H∥都被发现与用不同方法在VELA卫星上进行的测量是一致的。这些值小于1×10−2ergs/cm~2/s，已经足够低，需要修改太阳风理论中使用的斯皮策-哈姆电导率公式。
This paper describes studies of electrons between 10 ev and 9.9 kev in the solar wind. The transport of energy in the rest frame of the plasma is evaluated and shown to be parallel to the interplanetary magnetic field. The presence of electrons from solar events causes this energy-flux density E∥ to exceed the heat flow H∥ due to thermal electrons. In one such event, the observations are shown to be consistent with the solar-electron observations made at higher energies. When observations are made at a point connected to the earth's bow shock by an interplanetary-field line, a comparatively large energy flux along the field toward the sun is observed, but H∥ remains outwardly directed during this time interval. In either situation H∥ is found to be consistent with measurements made on Vela satellites by a different method. These values, less than 1×10−2 ergs/cm2/sec, are sufficiently low to require modifications to the Spitzer-Harm conductivity formula for use in solar-wind theories.