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Chromospheric Activity and Stellar Evolution

Published online by Cambridge University Press:  06 September 2019

Rudolf Kippenhahn
Rudolf Kippenhahn*
Affiliation:
Göttingen University Observatory

Extract

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Stellar evolution carries a star through the Hertzsprung-Russell-Diagram. For a given mass, M. one obtains both luminosity, L, and radius, R, as functions of time, t. From these parameters we determine the surface gravity and the effective temperature as functions of t:

g(t),Teff(t).

It is these two parameters which determine the properties of the outermost layers of a star, the atmosphere and the top of the hydrogen convective zone.

Type
Part IV: Variation of Chromospheric Properties with Stellar Mass and Age
Information
International Astronomical Union Colloquium , Volume 19: Stellar Chromospheres , February 1973 , pp. 263 - 278
Copyright
Copyright © Nasa 1972

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