The magnetic and thermodynamical structure of a coronal hole

Details The magnetic and thermodynamical structure of a coronal hole The magnetic and thermodynamical structure of a coronal hole

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...97..251o&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 97, June 1985, p. 251-266.

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5

Coronal Holes, Solar Corona, Solar Magnetic Field, Thermodynamics, Computational Astrophysics, Density Distribution, Magnetic Field Configurations, Plasma Acceleration, Temperature Distribution

Scientific paper

A nonpolytropic model of a polar coronal hole of 2-5 solar radii constructed. The main assumptions are: (1) the magnetic structure of the sun can be described by a combination of dipole-like and radial fields; (2) in the magnetically dominated region rho(nu sq/2) much less than B sq/8 pi the influence of the outflow on the magnetic structure is negligible. The magnetic and thermodynamic structures are obtained by solving the force balance equation for plasma with the observationally derived electron density. Profiles of velocities in the acceleration regime are presented and the influence of the outflow on the thermodynamic structure of the solar corona above the polar region is discussed.

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