Main Sequence Mass Loss and the Ages of Stars

The potentially observable consequences of the pulsation/rotation-induced mass loss from main-sequence A and F stars proposed by Willson et al. (1987) are discussed, reviewing the results of recent investigations. Particular attention is given to (1) evidence for a deficiency in A stars and an exces...

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Bibliographic Details
Published in:Annals of the New York Academy of Sciences 1989, Vol.571 (1), p.90-98
Main Author: WILLSON, L. A.
Format: Article
Language:English
Subjects:
640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
640107 - Astrophysics & Cosmology- Planetary Phenomena
AGE ESTIMATION
Astronomy
Astrophysics
CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS
Earth, ocean, space
Exact sciences and technology
MAIN SEQUENCE STARS
Mass loss and stellar winds
MASS TRANSFER
MATHEMATICAL MODELS
MODIFICATIONS
MOTION
ROTATION
SOLAR SYSTEM EVOLUTION
STAR CLUSTERS
STAR EVOLUTION
STARS
Stellar characteristics and properties
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Summary:The potentially observable consequences of the pulsation/rotation-induced mass loss from main-sequence A and F stars proposed by Willson et al. (1987) are discussed, reviewing the results of recent investigations. Particular attention is given to (1) evidence for a deficiency in A stars and an excess of F and G stars, as predicted by the theory, (2) cluster HR diagrams and age estimates, and (3) modifications to standard models of solar-system evolution. It is pointed out that the time scales and mass-loss rates required to explain the observed properties of clusters and field stars in this theory are the same as those needed to account for the early development of the solar system.
ISSN:0077-8923
1749-6632
DOI:10.1111/j.1749-6632.1989.tb50499.x