The thermal stability of solar coronal loops in hydrostatic equilibrium

Details The thermal stability of solar coronal loops in hydrostatic equilibrium The thermal stability of solar coronal loops in hydrostatic equilibrium

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...113..269w&link_type=abstract

Astronomy and Astrophysics, vol. 113, no. 2, Sept. 1982, p. 269-276. Research supported by the University of St. Andrews and Sc

Astronomy and Astrophysics

Astrophysics

10

Coronal Loops, Magnetohydrodynamic Stability, Magnetohydrostatics, Plasma Equilibrium, Thermal Stability, Equilibrium Equations, Gravitational Effects, Hydrostatic Pressure

Scientific paper

Many static models of solar coronal loops have been set up, and more recently there have been attempts to look at their stability. A loop is globally stable or unstable to thermal effects depending on whether the net conduction (stabilizing) or the net radiation (destabilizing) dominates. It has previously been found that uniform-pressure loops are unstable if the base heat flux is too small. In particular, thermally isolated loops are always unstable. In the present paper the effects of gravity are included by considering a basic state in hydrostatic equilibrium. It is found that the inclusion of gravity is a stabilizing influence because it lowers the density (and hence the radiation) in the upper parts of a loop. Thermally isolated loops are shown to be thermally unstable when they are short but stable when they are long enough. Thus, small coronal loops would be expected to exhibit dynamic fluctuations and longer ones to possess a steadier emission.

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