Towards a rigorous model for multifluid expansions of stellar coronae - Application to the solar wind

Details Towards a rigorous model for multifluid expansions of stellar coronae - Application to the solar wind Towards a rigorous model for multifluid expansions of stellar coronae - Application to the solar wind

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...241..187f&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 241, no. 1, Jan. 1991, p. 187-196. Research supported by DFG.

Astronomy and Astrophysics

Astrophysics

9

Astronomical Models, Magnetohydrodynamic Waves, Solar Wind, Stellar Coronas, Stellar Magnetic Fields, Interstellar Matter, Polarization (Waves), Subsonic Flow

Scientific paper

The existing standard MHD stellar wind models are extended here in two respects. First, the treatment of the thermal properties of electrons and protons is completed by numerical integration of two temperature equations describing for both constituents the components parallel and perpendicular to the magnetic field. Second, considering the motion of electrons and protons is separated by two corresponding momentum equations including mutual friction terms and the electric polarization field due to the different scale heights and expansion characteristics of the two species. The field - a generalization of the Pannekoek-Rosseland field - represents the main interaction mechanisms between electrons and protons and enables a first quantitative investigation of the subsonic character of solar wind electrons and of recently postulated upwind/downwind asymmetries in the solar wind connected with these. In spite of their mathematical complexity the relevant differential equations can be solved without inadequate numerical efforts.

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