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The Evolution of Stars to the White Dwarf Stage

Published online by Cambridge University Press:  25 April 2016

Gary Wegner
Gary Wegner*
Affiliation:
Mount Stromlo and Siding Spring Observatories The Australian National University
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Extract

That the parent masses of white dwarf (WD) stars can exceed the Chandrasekhar limit of approximately 1.2 can be seen from star clusters that have turn-off points in excess of this mass and still contain WD. Auer and Woolf argued that WD in the Hyades and Pleiades is evidence that stars with masses larger than 2.5 can become WD. Sandage and Jones have used the luminosity function to compute the number of WD expected in several clusters. Jones estimated that the brighter of the two WD sequences arises from stars of mass greater than 1-9 Schwarzschild, for example, has stressed the importance of a knowledge of the resulting mass-loss. Deutsch has discussed mass-loss from red giants and Faulkner has summarized the relationship between the planetary nebulae and the WD. Nevertheless, the role of WD formation in the enrichment of the interstellar medium and the relationship between WD and their parent stars is unclear.

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Contributions
Information
Publications of the Astronomical Society of Australia , Volume 2 , Issue 3 , October 1972 , pp. 153 - 154
Copyright
Copyright © Astronomical Society of Australia 1972

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References

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