Which magnetic storms produce relativistic electrons at geosynchronous orbit?

被引:197
作者
O'Brien, TP
McPherron, RL
Sornette, D
Reeves, GD
Friedel, R
Singer, HJ
机构
[1] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA
[2] Univ Calif Los Alamos Natl Lab, Los Alamos, NM 87544 USA
[3] NOAA, Space Environm Ctr, Boulder, CO 80305 USA
[4] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA USA
[5] Univ Nice, Nice, France
[6] CNRS, Phys Mat Condensee Lab, F-06034 Nice, France
关键词
D O I
10.1029/2001JA000052
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Relativistic electrons appear in the geosynchronous environment following some, but not all, geomagnetic storms. The ability to identify which storms produce these electrons would bring us much closer to explaining the mechanism responsible for their appearance, and it would provide the space weather community with a means to anticipate the electron hazard to geosynchronous spacecraft. We apply a recently developed statistical technique to produce an hourly time series of relativistic electron conditions at local noon along geosynchronous orbit using several geosynchronous monitors. We use a cross-correlation analysts to determine what parameters in the solar wind and magnetosphere might influence the Aux of relativistic electrons. We then perform a superposed epoch analysis to compare storms with and storms without the appearance of these electrons. We investigate a number of solar wind and magnetospheric parameters for these two sets of storms at 1-hour resolution, In particular, sustained solar wind velocity in excess of 450 km s(-1) is a strong external indicator of the subsequent appearance of relativistic electrons, :ln the magnetosphere, long-duration elevated Pc 5 ULF wave power during the recovery phase of magnetic storms appears to discriminate best between those storms that do and do not produce relativistic electrons.
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页码:15533 / 15544
页数:12
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