Origin of hot and high speed plasmas in plasma sheet: plasma acceleration and heating due to slow shocks

Details Origin of hot and high speed plasmas in plasma sheet: plasma acceleration and heating due to slow shocks Origin of hot and high speed plasmas in plasma sheet: plasma acceleration and heating due to slow shocks

Sep 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997adspr..20..973h&link_type=abstract

Advances in Space Research, Volume 20, Issue 4-5, p. 973-982.

Physics

2

Scientific paper

The origin of hot and high speed plasmas observed by the GEOTAIL spacecraft in the magnetotail is discussed in terms of slow shock acceleration and heating. We find that the bulk flow energy for the hot and high speed plasma in the tail plasma sheet is larger than the thermal energy, and there is an lower limit on the ratio of the thermal to bulk flow energy 2p/rhov^2. The lower boundary of 2p/rhov^2 is about 0.2 - 0.4, and the ratio is independent of the plasma temperature in the range of several 100 eV to 10 keV. It is believed that the magnetic reconnection associated with a slow shock can produce the hot and high speed plasma, though the observed lower limit cannot be explained by a standard slow shock heating and acceleration process, because the lower limit of 2p/rhov^2 obtained by the standard slow shock Rankine-Hugoniot relation is 0.4 even for the strong slow shock limit. In order to explain the observed lower boundary of 2p/rhov^2, we study the Rankine-Hugoniot relations by taking into account of non-standard MHD effects such as a temperature anisotropy and a heat flux. The observed lower limit can be explained by a slow shock including the temperature anisotropy and the heat flux effects.

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