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The Distribution of Chromospheric Emission Strengths Among Red Dwarfs

Published online by Cambridge University Press:  12 April 2016

David R. Soderblom
David R. Soderblom*
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts USA

Extract

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The survey of Vaughan and Preston (1980, hereafter VP) of Ca II emission among solar neighborhood stars has shown the distribution of chromospheric emission (CE) of these stars. For stars bluer than (B-V)= 1.50, it is possible to transform VP's equivalent width S into a relative flux by use of Middelkoop's (1982) formulae. This enables construction of a chromospheric color-magnitude diagram (illustrated in Soderblom 1982), which shows the same general features as VP's log S vs. (B-V) plot, except that the CE (as a fraction of the stellar luminosity) declines with mass due to the decline of the ZAMS rotational velocity with mass (Soderblom 1983).

Type
Session I: General Characteristics of Active Dwarfs
Information
International Astronomical Union Colloquium , Volume 71: Activity in Red-Dwarf Stars , 1983 , pp. 67 - 70
Copyright
Copyright © Reidel 1983

References

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