Self consistent MHD modeling of the solar wind from polar coronal holes

Details Self consistent MHD modeling of the solar wind from polar coronal holes Self consistent MHD modeling of the solar wind from polar coronal holes

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..145s&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 145

Physics

1

Particle Emission, Solar Wind, Magnetohydrodynamics And Plasmas, Magnetohydrodynamic And Fluid Equation

Scientific paper

We have developed a 2D self consistent MHD model for solar wind flow from antisymmetric magnetic geometries. We present results in the case of a photospheric magnetic field which has a dipolar configuration, in order to investigate some of the general characteristics of the wind at solar minimum. As in previous studies, we find that the magnetic configuration is that of a closed field region (a coronal helmet belt) around the solar equator, extending up to about 1.6 Rsolar, and two large open field regions centred over the poles (polar coronal holes), whose magnetic and plasma fluxes expand to fill both hemispheres in interplanetary space. In addition, we find that the different geometries of the magnetic field lines across each hole (from the almost radial central polar lines to the highly curved border equatorial lines) cause the solar wind to have greatly different properties depending on which region it flows from. We find that, even though our simplified model cannot produce realistic wind values, we can obtain a polar wind that is faster, less dense and hotter than equatorial wind, and found that, close to the Sun, there exists a sharp transition between the two wind types. As these characteristics coincide with observations we conclude that both fast and slow solar wind can originate from coronal holes, fast wind from the centre, slow wind from the border.

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