Thermal stability of static coronal loops. I - Effects of boundary conditions

Details Thermal stability of static coronal loops. I - Effects of boundary conditions Thermal stability of static coronal loops. I - Effects of boundary conditions

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...298..876a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 298, Nov. 15, 1985, p. 876-886. Previously announced in STAR as N85-22330.

Astronomy and Astrophysics

Astrophysics

28

Boundaries, Boundary Conditions, Chromosphere, Coronal Loops, Perturbation Theory, Solar Corona, Stellar Models, Density (Mass/Volume), Perturbation, Pressure, Solar Temperature

Scientific paper

The linear stability of static coronal-loop models undergoing thermal perturbations was investigated. The effect of conditions at the loop base on the stability properties of the models was considered in detail. The question of appropriate boundary conditions at the loop base was considered and it was concluded that the most physical assumptions are that the temperature and density (or pressure) perturbations vanish there. However, if the base is taken to be sufficiently deep in the chromosphere, either several chromospheric scale heights or several coronal loop lengths in depth, then the effect of the boundary conditions on loop stability becomes negligible so that all physically acceptable conditions are equally appropriate. For example, one could as well assume that the velocity vanishes at the base. The growth rates and eigenmodes of static models in which gravity is neglected and in which the coronal heating is a relatively simple function, either constant per-unit mass or per-unit volume were calculated. It was found that all such models are unstable with a growth rate of the order of the coronal cooling time. The physical implications of these results for the solar corona and transition region are discussed.

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