Thermal equilibria in solar coronal magnetic loops: Gravitational considerations

Details Thermal equilibria in solar coronal magnetic loops: Gravitational considerations Thermal equilibria in solar coronal magnetic loops: Gravitational considerations

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..291s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 1, p. 291-303

Physics

6

Equilibrium, Gravitational Effects, Magnetic Fields, Solar Corona, Solar Physics, Stellar Models, Sun, Thermal Emission, Critical Point, Equations Of State, High Temperature Plasmas, Magnetostatics, Solar Heating, Solar Prominences

Scientific paper

Equations of thermal equilibria along coronal magnetic loops (with constant cross-sectional area) are solved in the absence and the presence of gravity. When the effect of gravity is negligible, loops may exist with cool summits; these loops consist of two portions, an isothermal portion at the summit and a non-isothermal portion near the footpoint. In the presence of gravity, the two-component structure no longer exists and there is a restriction (dependent on the heating) on the lengths of loops with cool summits. Loops with hot summits are cooled slightly by the incorporation of gravity. A model of a cylindrical arcade is set up where the heating and the magnetic field vary with position. Hot arcades exist as do arcades with a vertical cool sheet surrounded by hotter plasma - a situation that occurs for a prominence. It is anticipated that loops with cool summits may exist for higher values of gravity when the loop area is allowed to vary with position.

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