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Magnetic field-related heating instabilities in the surface layers of the sun and starsThe 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.
Document ID
19830035800
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Ferrari, A.
(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; CNR, Istituto di Cosmo-Geofisica; Torino, Universita Turin, Italy)
Rosner, R.
(Harvard-Smithsonian Center for Astrophysics Cambridge, MA, United States)
Vaiana, G. S.
(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA; Osservatorio Astronomico Palermo, Italy)
Date Acquired
August 11, 2013
Publication Date
December 15, 1982
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
83A17018
Funding Number(s)
CONTRACT_GRANT: NAGW-79
Distribution Limits
Public
Copyright
Other

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