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Evolution of stars decreasing in mass

Published online by Cambridge University Press:  14 August 2015

A. G. Massevitch
A. G. Massevitch*
Affiliation:
Sternberg Astronomical Institute, Moscow

Extract

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By a “steady” evolution of a star is understood such a change of its main parameters in the flow of time, which occurs in the range of an assumed equilibrium model and is caused by regular interior processes. So, for instance, the gradual conversion of hydrogen into helium in the convective core of a star, whose substance is not mixed fully, leads to a continuous change of its luminosity, radius, Tc and ρc, convective core dimensions. However, all these changes occur all the time in the limits of the model's state of equilibrium, and the structure of the star (radiative envelope and convective core) remains unchanged until a certain limit is reached in the ratio.

Type
II. Theoretical Interpretations of the Hertzsprung-Russell Diagram
Information
Symposium - International Astronomical Union , Volume 10: The Hertzsprung-Russell Diagram , 1959 , pp. 89 - 98
Copyright
Copyright © CNRS 1959 

References

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