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Heating of solar and stellar chromospheres and coronae by MHD wavesThe two general classes of models that deal with the required heating of stellar chromospheres and coronae assume that outer stellar atmospheres are heated by hydrodynamic or by magnetohydrodynamic (MHD) waves and that these waves are generated by turbulent motions in the stellar convection zones. This paper considers the types of MHD waves and the source of these waves in stars like sun, the efficiency of the generation of MHD waves, and the manner of propagation and energy dissipation of MHD waves. It is shown that the basic criteria for the validity of any theory of MHD wave heating must account for the mean level of heating observed in stellar chromospheres and coronae, and for the range of radiative losses observed for a given spectral type. It is also required that the MHD wave heating theory accounts for the existence of inhomogeneities in stellar atmospheres. The results obtained indicate that magnetic tube waves might supply enough energy for the chromospheric and coronal heating and might also account for the observed range of variations of stellar radiative losses for a given spectral type.
Document ID
19930042161
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Musielak, Z. E.
(Alabama Univ. Huntsville, United States)
Date Acquired
August 16, 2013
Publication Date
January 1, 1992
Publication Information
Publication: Societa Astronomica Italiana, Memorie
Volume: 63
Issue: 4-Mar
ISSN: 0037-8720
Subject Category
Astrophysics
Accession Number
93A26158
Funding Number(s)
CONTRACT_GRANT: NAG8-839
CONTRACT_GRANT: NATO-CRG-0058/91
Distribution Limits
Public
Copyright
Other

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