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A Fibril Structure Model for Stellar Prominences

Published online by Cambridge University Press:  12 April 2016

R. Oliver  and
J.L. Ballester
R. Oliver
Affiliation:
Departament de Física, Universitat de les Illes Balears, E-07071 Palma de Mallorca, Spain
J.L. Ballester
Affiliation:
Departament de Física, Universitat de les Illes Balears, E-07071 Palma de Mallorca, Spain

Abstract

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Extensive observational background exists about the presence of cool material clouds embedded in the stellar coronae of rapidly rotating, late-type stars. Observations of such clouds in HKAqr (Gliese 890) and HD 197890 suggest that the clouds are at heights smaller than the star’s corotation radius and could be looked at as a phenomenon similar to that of solar prominences. Recent observations of solar prominences have reinforced the evidence about their fibril structure made of many long, thin magnetic flux tubes making angles about 25 degrees with the direction of the filament channel, with only the central 10–20% of the magnetic flux tubes filled with cool matter, which can produce a depression at the summits of the flux tubes. Then, assuming a similar structure for the stellar cool clouds, we have looked for the physical characteristics of such stellar prominences, i.e. the size of the flux tube depression, the density, temperature, half-width and supported mass of the cool region, taking into account gravity variation with height and centrifugal acceleration, since such clouds have been detected at great heights within stellar coronae belonging to rapid rotators.

Type
Stellar Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 247 - 250
Copyright
Copyright © Astronomical Society of the Pacific 1998

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