The Global Solar Wind Between 1 AU and the Termination Shock

Details The Global Solar Wind Between 1 AU and the Termination Shock The Global Solar Wind Between 1 AU and the Termination Shock

Apr 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...713..721w&link_type=abstract

The Astrophysical Journal, Volume 713, Issue 2, pp. 721-730 (2010).

Astronomy and Astrophysics

Astronomy

1

Magnetic Fields, Magnetohydrodynamics: Mhd, Plasmas, Solar Wind

Scientific paper

This paper studies the global solar wind between 1 AU and the termination shock, taking into account the highly latitude dependent solar wind at the 1 AU boundary and the ionization of interstellar neutral hydrogen. A system of two-fluid magnetohydrodynamics equations governs the flow of solar wind plasma; the conditions of the solar wind at 1 AU are generated from Ulysses data for the relatively stable state of the wind during the declining phase and solar minimum of the solar cycle. A one-fluid model is used to describe the flow of neutral hydrogen and its condition in the far-field boundary outside the termination shock. Simultaneous solutions are obtained using a high-resolution computational code for the two equation systems coupled by the ionization of neutral hydrogen. The ionization process leads to removal of neutral hydrogen in the heliosphere: a hydrogen cavity forms inside ~4 AU; the cavity extends on the downwind side to form a long cavity wake. Solutions show how the ionization process and the wind condition at 1 AU boundary affect the spatial variation of the wind speed, temperature, pickup proton, fast Mach number, and plasma β-ratio. The wind properties inside 4 AU are axisymmetrical about the solar rotation axis; this axi-symmetry totally disappears in the outer heliosphere. All wind properties are substantially modified at an increasing heliocentric distance on the upwind side to generate an upwind-downwind asymmetry dictated by the direction of the relative motion between the Sun and the interstellar medium.

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