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Chromospheric heating in late–type stars: evidence for magnetic and nonmagnetic surface structure

Published online by Cambridge University Press:  25 May 2016

Manfred Cuntz
Manfred Cuntz*
Affiliation:
Joint Institute for Laboratory Astrophysics University of Colorado and NIST Boulder, CO 80309-0440, USA

Abstract

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The aim of this paper is to evaluate recent observational and theoretical results concerning the physics of chromospheric heating as inferred from IUE, HST-GHRS and ROSAT data. These results are discussed in conjunction with theoretical model calculations based on acoustic and magnetic heating to infer some conclusions about the magnetic and nonmagnetic surface structure of cool luminous stars. I find that most types of stars may exhibit both magnetic and nonmagnetic structures. Candidates for pure nonmagnetic surface structure include M-type giants and supergiants. M-type supergiants are also ideal candidates for identifying direct links between the appearance of hot spots on the stellar surface (perhaps caused by large convective bubbles) and temporarily increased chromospheric heating and emission.

Type
Session IV: “Outer Atmospheric Structure”
Information
Symposium - International Astronomical Union , Volume 176: Stellar Surface Structure , 1996 , pp. 393 - 402
Copyright
Copyright © Kluwer 1996 

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