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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Constraining Suprathermal Electron Evolution in a Parker Spiral Field With Cassini Observations
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Constraining Suprathermal Electron Evolution in a Parker Spiral Field With Cassini Observations

机译：约束Suprathermal电子在进化帕克与卡西尼号的观察螺旋场

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摘要

Suprathermal electrons in the solar wind consist of the "halo," present at all pitch angles, and the "strahl" which is a field-aligned, beam-like population. Examining the heliospheric evolution of strahl beams is key to understanding the in-transit processing of solar wind suprathermal electrons, in particular, to identify electron scattering mechanisms and to establish the origin of the halo population. Not only does this have significant implications with regard to the kinetic processes occurring within the solar wind but also its thermodynamic evolution, as the suprathermal electrons carry the majority of the solar wind heat flux. In this investigation, an established model for suprathermal electron evolution in a Parker spiral interplanetary magnetic field is adapted from its original use. The model is constrained using solar wind strahl observed by the Cassini mission on its interplanetary journey to Saturn. The effects of large scale IMF geometry due to different solar wind velocities and application of different electron scattering factors are examined. It is found that slow solar wind speeds provide the closest match to the strahl width observations, both in terms of radial distance and electron energy trends, and that predominantly slower solar wind speeds were therefore likely observed by the Cassini mission en-route to Saturn. It is necessary to include a strahl scattering factor which increases with electron energy in order to match observations, indicating that the strahl scattering mechanism must have an inherent energy dependence.
机译：太阳风由Suprathermal电子的“光环”,出席所有螺距角,和“特拉”这是一个field-aligned,射线人口。特拉梁是理解的关键在途的太阳风suprathermal的处理特别是电子,电子识别散射机制和建立原点人口的光环。关于重要的影响太阳风中的动力学过程而且其热力学进化,suprathermal电子携带的大部分太阳风热流。建立模型suprathermal电子在帕克螺旋星际演化磁场是改编自原来的使用。该模型使用太阳风strahl约束由卡西尼任务在其观察星际之旅土星。大规模的国际货币基金组织(IMF)几何由于不同的太阳能风速度和不同的应用电子散射因素研究。发现缓慢太阳风速度提供strahl宽度的观察,最近的比赛对于径向距离和电子主要能源的趋势,而且慢太阳风速度因此有可能观察到卡西尼任务动身前往土星。从而增加电子能量为了吗比赛的观察,表明特拉必须有一个内在的能量散射机制依赖。

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