Modeling of the tail region of the heliospheric interface

Details Modeling of the tail region of the heliospheric interface Modeling of the tail region of the heliospheric interface

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..218a&link_type=abstract

SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 218-2

Physics

4

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind

Scientific paper

The processes in the tail region of the interaction of the solar wind with the partially ionized local interstellar medium are investigated in a framework of the self-consistent kinetic gas dynamic model. It is shown that charge exchange of the hydrogen atoms with the plasma protons leads to suppression of the gas dynamic instabilities and disappearance the contact discontinuity at sufficiently large distances from the Sun. It is shown that the solar wind plasma temperature decreases and, ultimately, the parameters of the plasma and hydrogen atoms approach to the corresponding parameters of the pristine interstellar medium at large heliocentric distances.

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