Magnetic field-related heating instabilities in the surface layers of the sun and stars

Details Magnetic field-related heating instabilities in the surface layers of the sun and stars Magnetic field-related heating instabilities in the surface layers of the sun and stars

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263..944f&link_type=abstract

Astrophysical Journal, Part 1, vol. 263, Dec. 15, 1982, p. 944-951. Research supported by the Consiglio Nazionale delle Ricerch

Astronomy and Astrophysics

Astrophysics

15

Chromosphere, Magnetohydrodynamic Stability, Solar Corona, Stellar Coronas, Stellar Magnetic Fields, Surface Layers, Atmospheric Heating, Cold Plasmas, Equilibrium Equations, Main Sequence Stars, Rarefied Plasmas, Solar Atmosphere, Solar Magnetic Field

Scientific paper

The stability of a magnetized low-density plasma to current-driven filamentation instabilities is investigated and the results are applied to the surface layers of stars. Unlike previous studies, the initial (i.e., precoronal) state of the stellar surface atmosphere is taken to be a low-density, optically thin magnetized plasma in radiative equilibrium. The linear analysis shows that the surface layers of main-sequence stars (including the sun) which are threaded by magnetic fields are unstable; the instabilities considered lead to structuring perpendicular to the ambient magnetic fields. These results suggest that relatively modest surface motions, in conjunction with the presence of magnetic fields, suffice to account for the presence of inhomogeneous chromospheric and coronal plasma overlying a star's surface.

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