The stability of solar coronal loops

Details The stability of solar coronal loops The stability of solar coronal loops

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...232l.125a&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 232, Sept. 1, 1979, p. L125-L129.

Astronomy and Astrophysics

Astrophysics

66

Magnetohydrodynamic Stability, Solar Corona, Solar X-Rays, Stellar Models, Eigenvalues, Equilibrium Equations, Perturbation Theory, Plasma Equilibrium

Scientific paper

The stability of the 'quasi-static' models of coronal loops was examined. It was found that all models in which the heat flux at the base of the loop is assumed to vanish are unstable to the growth of thermal perturbations. The growth rates and the profiles of the unstable modes indicate that the instability involves primarily the low-temperature, transition-region plasma. The models can be made stable only by assuming that the heat flux at the base of the loop is large, of the order of 13% of the maximum flux in the loop. The results imply that the transition region must be intrinsically dynamic.

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