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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Statistical study of chorus wave distributions in the inner magnetosphere using Ae and solar wind parameters
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Statistical study of chorus wave distributions in the inner magnetosphere using Ae and solar wind parameters

机译：合唱波分布的统计研究内磁层使用Ae和太阳风参数

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摘要

Energetic electrons within the Earth’s radiation belts represent a serious hazard to geostationary satellites. The interactions of electrons with chorus waves play an important role in both the acceleration and loss of radiation belt electrons. The common approach is to present model wave distributions in the inner magnetosphere under different values of geomagnetic activity as expressed by the geomagnetic indices. However, it has been shown that only around 50% of geomagnetic storms increase flux of relativistic electrons at geostationary orbit while 20% causes a decrease and the remaining 30% has relatively no effect. This emphasizes the importance of including solar wind parameters such as bulk velocity (V), density (n), flow pressure (P), and the vertical interplanetary magnetic field component (Bz) that are known to be predominately effective in the control of high energy fluxes at the geostationary orbit. Therefore, in the present study the set of parameters of the wave distributions is expanded to include the solar wind parameters in addition to the geomagnetic activity. The present study examines almost 4 years (1 January 2004 to 29 September 2007) of Spatio-Temporal Analysis of Field Fluctuation data from Double Star TC1 combined with geomagnetic indices and solar wind parameters from OMNI database in order to present a comprehensive model of wave magnetic field intensities for the chorus waves as a function of magnetic local time, L shell (L), magnetic latitude (λ_m), geomagnetic activity, and solar wind parameters. Generally, the results indicate that the intensity of chorus emission is not only dependent upon geomagnetic activity but also dependent on solar wind parameters with velocity and southward interplanetary magnetic field Bs (Bz < 0), evidently the most influential solar wind parameters. The largest peak chorus intensities in the order of 50 pT are observed during active conditions, high solar wind velocities, low solar wind densities, high pressures, and high Bs. The average chorus intensities are more extensive and stronger for lower band chorus than the corresponding upper band chorus.
机译：高能电子在地球的辐射对同步带代表一个严重的威胁卫星。在合唱波发挥重要作用加速度和辐射带的损失电子。波分布的模型磁气圈在不同的值所表达的地磁活动地磁指数。只有大约50%的地磁风暴增加的相对论性电子通量地球静止轨道而导致减少20%和剩下的30%相对没有效果。这强调了包括太阳能的重要性风参数如散装速度(V),密度(n),流压力(P)和垂直行星际磁场组件(Bz)已知的主要有效吗控制的高能通量地球静止轨道。研究波的参数设置分布是扩大到包括太阳能除了地磁风参数活动。年(2004年1月1日到2007年9月29日)场波动的时空分析数据从双星TC1结合地磁指数和太阳风参数从数据库泛光灯来呈现一个综合模型的波磁场合唱的强度的函数当地时间磁,L壳(左),磁纬度(λ_m)、地磁活动和太阳能风参数。合唱排放不仅强度还依赖于地磁活动依赖于太阳风参数与速度向南和行星际磁场Bs(Bz < 0),显然是最具影响力的太阳能风参数。强度的顺序50 pT在活跃的条件下,高的太阳风太阳风速度、低密度、高压力,和高Bs。强度更广泛、更强乐队合唱低于相应的上层乐队合唱。

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