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Evolution of 1–5 Mm⊙ Stars by Mass Loss

Published online by Cambridge University Press:  07 August 2017

E. Vassiliadis  and
P.R. Wood
E. Vassiliadis
Affiliation:
Mount Stromlo and Siding Spring Observatories, Private Bag, Weston Creek P.O., Canberra, ACT 2611, Australia
P.R. Wood
Affiliation:
Mount Stromlo and Siding Spring Observatories, Private Bag, Weston Creek P.O., Canberra, ACT 2611, Australia

Extract

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Stars of mass 1–5 MM⊙ and composition Y=0.25 and Z=0.016 have been evolved from the main-sequence to the white dwarf stage with an empirical mass loss formula based on observations of mass loss rates in AGB stars. This mass loss formula (Wood 1990) causes the mass loss rate to rise exponentially with pulsation period on the AGB until superwind rates are achieved, where these rates correspond to radiation pressure driven mass loss rates. The formula was designed to reproduce the maximum periods observed for optically-visible LPVs and it also reproduces extremely well the maximum AGB luminosities observed in star clusters in the Magellanic Clouds (see Vassiliadis and Wood 1992 for details).

Type
V. Planetary Nebulae Connection: Evolution to White Dwarfs
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 478
Copyright
Copyright © Kluwer 1993 

References

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Vassiliadis, E. and Wood, P.R. 1992, in preparation.Google Scholar
Wood, P.R. 1990, in From Miras to Planetary Nebulae , eds. Mennessier, M.O. and Omont, A. (Editions Frontières), p. 67.Google Scholar
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