Structure of Slow Shocks in the Presence of Heat Conduction

Details Structure of Slow Shocks in the Presence of Heat Conduction Structure of Slow Shocks in the Presence of Heat Conduction

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11a0699t&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH11A-0699

Other

2139 Interplanetary Shocks, 2788 Storms And Substorms, 7509 Corona, 7835 Magnetic Reconnection, 7851 Shock Waves

Scientific paper

The structure of slow shock in the presence of a heat conduction parallel to the local magnetic field is simulated from the set of MHD equations. In our study, a pair of slow shocks is formed through the evolution of a current sheet initiated by the presence of a normal magnetic field. It is found that the slow shock consists of two parts: the isothermal main shock and foreshock. Significant jumps in plasma density, velocity and magnetic field occur across the main shock, but the temperature is found to be continuous across the main shock. The foreshock is featured by a smooth temperature variation and is formed due to the heat flow from downstream to upstream region. %In the foreshock region the plasma temperature and pressure are enhanced, while the plasma density remains nearly constant. The plasma density downstream of the main shock decreases with time, while the downstream temperature increases with time, keeping the downstream pressure constant. It is shown that the jumps in plasma density, pressure, velocity, and magnetic field across the main shock are determined by the set of modified isothermal Rankine-Hugoniot conditions. It is also found that a jump in the temperature gradient is present across the main shock in order to satisfy the energy conservation. The present results can be applied to the heating in the solar corona and solar wind.

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