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Quiescent chromospheric response to the (E)UV/optical flare radiation field on dMe stars

Published online by Cambridge University Press:  23 September 2016

E. R. Houdebine  and
C. J. Butler
E. R. Houdebine
Affiliation:
1 Institut d'Astrophysique Spatiale, Univ. d'Orsay, bt. 120, 91400 Orsay, France
C. J. Butler
Affiliation:
2 Armagh Observatory, Armagh, BT61 9DG, N. Ireland

Abstract

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We examine the response of the quiescent chromosphere to the large (E)UV and optical continuum and spectral line radiation field arising from a flare. We show that during a UV Ceti type flare, which displays a large U-band enhancement, a major part of the Balmer line flux may arise from the “quiescent chromosphere”, rather than the heated flare plasma itself. This leads us to distinguish two main phases in the Balmer lines, as first proposed by Houdebine et al. (1989): an early, mainly impulsive, phase, driven by radiative pumping of the quiescent chromosphere, which is mainly correlated with continuum variations, and a later one, related to the thermal flare phase, which arises from the cooling of the flare plasma itself. The effect of the radiative pumping is much larger for stellar (dMe) than for solar flares, due to substantial differences in the flare, relative to the quiescent, level and the quiescent chromospheric density and temperature.

Type
IV Theoretical Problems and Interpretation of Observations
Information
Symposium - International Astronomical Union , Volume 137: Flare Stars in Star Clusters, Association and Solar Vicinity , 1990 , pp. 313 - 316
Copyright
Copyright © Kluwer 1990 

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