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The Magnetic Field Configuration in Solar and Stellar Chromospheres

Published online by Cambridge University Press:  04 August 2017

U. Anzer  and
D.J. Galloway
U. Anzer
Affiliation:
Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1, 8046 Garching, FRG
D.J. Galloway
Affiliation:
Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1, 8046 Garching, FRG

Abstract

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Calculations are presented for the inhomogeneous magnetic field structure above a stellar photosphere which has magnetic flux tubes located at the downdraughts of its supergranulation pattern. Regions can be delineated where the ambient magnetic energy density is large or small compared with the thermal energy density derived from a model atmosphere. This enables the relative importance of magnetic versus non-magnetic heating mechanisms to be assessed. For the quiet Sun, over half the chromospheric emission must be supplied non-magnetically, whilst the network and active regions require a magnetic supply. For other late-type stars, a simple working rule suggests that when the magnetic field is strong enough to be directly observable, the chromosphere will be magnetically dominated.

Type
IV. The Role of Magnetic Fields in the Structure and Energy Balance of Stellar Atmospheres
Information
Symposium - International Astronomical Union , Volume 102: Solar and Stellar Magnetic Fields: Origins and Coronal Effects , 1983 , pp. 339 - 344
Copyright
Copyright © Reidel 1983 

References

Anzer, U. and Galloway, D.J.: 1982, to appear in Mon. Not. Roy. Astron. Soc. Google Scholar
Avrett, E.H.: 1981, in “Solar Phenomena in Stars and Stellar Systems”, ed. Bonnet, R.M. and Dupree, A.K. (Reidel), p. 173.CrossRefGoogle Scholar
Ayres, T.R. and Linsky, J.L.: 1975, Astrophys. J. 200, p. 660.Google Scholar
Gabriel, A.H.: 1976, Phil. Trans. Roy. Soc. London A281, p. 339.Google Scholar
Giovanelli, R.G. and Jones, H.P.: 1982, preprint.Google Scholar
Kopp, R.A. and Kuperus, M.: 1968, Solar Phys. 4, p. 212.Google Scholar
Newkirk, G. Jr. and Harvey, J.W.: 1968, Solar Phys. 3, p. 321.Google Scholar
Robinson, R.D., Worden, S.P., and Harvey, J.W.: 1980, Astrophys. J. 236, p. L155.Google Scholar
Simon, G.W., Weiss, N.O., and Nye, A.: 1982, preprint.Google Scholar
Stenflo, J.O.: 1982, Solar Phys. 80, p. 209.Google Scholar
Ulmschneider, P.: 1981, in “Solar Phenomena in Stars and Stellar Systems”, ed. Bonnet, R.M. and Dupree, A.K. (Reidel), p. 239.Google Scholar
Ulmschneider, P. and Stein, R.F.: 1982, Astron. Astrophys. 106, p. 9.Google Scholar
Vernazza, J.E., Avrett, E.H., and Loeser, R.: 1981, Astrophys. J. Suppl. 45, p. 635.Google Scholar