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Heating of Stellar Chromospheres and Transition Regions

Published online by Cambridge University Press:  26 May 2016

Zdzislaw E. Musielak
Zdzislaw E. Musielak*
Affiliation:
Department of Physics, University of Texas at Arlington, Arlington, TX 76019, USA email: zmusielak@uta.edu

Abstract

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To explain the heating of stellar chromospheres and transition regions, two classes of heating mechanisms have been considered: dissipation of acoustic and magnetic waves generated in stellar convection zones; and dissipation of currents generated by photospheric motions of surface magnetic fields. The focus of this paper is on the wave heating mechanisms and on recent results which demonstrate that theoretical models of stellar chromospheres based on the wave heating can explain the “basal flux” and the observed Ca II emission in most stars but cannot account for the observed Mg II emission in active stars. The obtained results clearly show that the base of stellar chromospheres is heated by acoustic waves, the heating of the middle and upper chromospheric layers is dominated by magnetic waves associated with magnetic flux tubes, and that other non-wave heating mechanisms are required to explain the structure of the highest layers of stellar chromospheres and transition regions.

Type
Part 9: Heating of Solar and Stellar Coronae
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 437 - 448
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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