Response of the midtail electric field to enhanced solar wind energy input

Details Response of the midtail electric field to enhanced solar wind energy input Response of the midtail electric field to enhanced solar wind energy input

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jgr...10417299n&link_type=abstract

Journal of Geophysical Research, Volume 104, Issue A8, p. 17299-17310

Physics

9

Magnetospheric Physics: Auroral Phenomena, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Magnetospheric Physics: Storms And Substorms

Scientific paper

We study the response of midtail plasma and field parameters to enhanced solar wind electric field input for two substorm intervals on November 22, 1995. The solar wind input signatures were quite different for these two substorms, which had major Pi2 onsets at 1108 and 1502 UT. The solar wind input for the 1108 UT substorm had a short timescale (~0.5 hour) electric field enhancement up to 1.5 mV/m, whereas the solar wind electric field for the 1502 UT substorm continuously exceeded 1.5 mV/m for ~2 hours. In association with the expansion phase onsets of both substorms, the electric field fluctuation in the midtail plasma sheet commenced. The electric field disturbances lasted for a time interval close to the length of time, in which the solar wind electric field was enhanced. The midtail plasma sheet electric field responded well to the enhanced solar wind input with a time delay of 45-80 min. The pressure decrease, which started at the onset of both substorms, ended quite differently for these two substorms: the pressure decreased until it approached the quiet time level in the course of the 1108 UT substorm, whereas the pressure dropped below the quiet time level during the expansion phase of the 1502 UT substorm and stayed at this low level until late in the recovery phase. Using polar cap potential drop and the pressure profile in the midtail, we estimate the relationship between the dayside and nightside potential drop. We suggest that the difference in the nightside flux transport rate could control the configuration of the midtail and could explain why the tail pressure responded differently during the expansion and recovery phase of the two substorms.

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