Numerical modeling of the halo electrons in the fast solar wind

Details Numerical modeling of the halo electrons in the fast solar wind Numerical modeling of the halo electrons in the fast solar wind

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jgra..108.1371c&link_type=abstract

Journal of Geophysical Research, Volume 108, Issue A10, pp. SSH 7-1, CiteID 1371, DOI 10.1029/2003JA009957

Physics

Plasma Physics

2

Interplanetary Physics: Solar Wind Plasma, Space Plasma Physics: Numerical Simulation Studies, Space Plasma Physics: Kinetic And Mhd Theory, Space Plasma Physics: Transport Processes

Scientific paper

A one-dimensional magnetohydrodynamic solar wind model is constructed to describe the behavior of the halo electrons in the fast electron-proton solar wind, assuming that the electrons are composed of two populations: the core and halo. The halo component is separated from the core electrons by increasing the heat deposition. It is shown that the model including only Coulomb collisions yields a much faster halo drift than observed if the halo temperature is in agreement with measured values. This supports the previous argument that some anomalous frictional processes caused by microinstabilities and/or wave-particle interactions exist in the solar wind. We show that these anomalous frictional processes can be approximated by enhanced Coulomb collisions together with a heat deposition that has a very large damping length. We find that beyond a certain heliocentric distance, say 20 RS, the anomalous frictional forces acting on the halo population are more important than the electric field force and the Coulomb collisional forces and become the dominant factor inhibiting the core-halo drift.

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