X line distribution determined from earthward and tailward convective bursty flows in the central plasma sheet

Details X line distribution determined from earthward and tailward convective bursty flows in the central plasma sheet X line distribution determined from earthward and tailward convective bursty flows in the central plasma sheet

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jgra..11506218z&link_type=abstract

Journal of Geophysical Research, Volume 115, Issue A6, CiteID A06218

Physics

Magnetospheric Physics: Magnetic Reconnection (7526, 7835), Magnetospheric Physics: Magnetotail, Magnetospheric Physics: Plasma Sheet, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Magnetospheric Physics: Substorms

Scientific paper

With TC-1, Cluster, and Geotail observations, we statistically analyzed earthward and tailward convective bursty flows (CBFs) from 7 to 31 RE to understand the distribution of X lines in the magnetotail. We also analyzed the effect of the solar wind condition on the X lines with ACE satellite observations. The statistical results show that the earthward CBFs can be distributed widely, from 7 to 31 RE. TC-1 exploration shows that tailward CBFs with negative Bz in the central plasma sheet can seldom be observed inside 13 RE. Tailward CBFs with negative Bz are mainly distributed outside 17 RE, thus indicating that near-Earth X lines are most likely to occur outside 17 RE. According to Cluster observations, the occurrence of tailward CBFs has a sudden increase from 17 to 19 RE. Geotail observations show a slow increase of tailward CBFs outside 20 RE. Both Cluster and Geotail observations indicate that the near-Earth X lines could occur inside 20 RE. The solar wind condition has a significant effect on the occurrence of the X line in the magnetotail. The occurrence of the X line can increase under strong solar wind and decrease under weak solar wind.

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