Mass loss towards the white dwarf stage

Details Mass loss towards the white dwarf stage Mass loss towards the white dwarf stage

Aug 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....59..411w&link_type=abstract

Astronomy and Astrophysics, vol. 59, no. 3, Aug. 1977, p. 411-418.

Astronomy and Astrophysics

Astrophysics

76

Angular Momentum, Stellar Evolution, Stellar Mass Ejection, White Dwarf Stars, Pleiades Cluster, Stellar Models, Supernovae

Scientific paper

White-dwarf mass distribution functions and mass-loss curves are computed using several different existing formulas and are compared with observational data for various white dwarfs. The comparison stars include LB 1497 in the Pleiades, 40 Eri B, EG 130, and EG 178 in the Sirius group, seven Hyades white dwarfs, and two non-DA stars. A number of cases are found in which mass loss toward the white-dwarf stage has been larger than predicted by current mass-loss formulas combined with evolutionary calculations for nonrotating single stars. Evidence for differential mass loss on a much larger scale than hitherto assumed is presented as an explanation of the horizontal branch, and a correlation between angular momentum and mass loss is proposed. It is suggested that high angular momentum is associated with large mass-loss rates, enabling even massive stars to become white dwarfs, and that low angular momentum is associated with small mass-loss rates, which may lead to supernova explosions. It is concluded that there is no fixed upper limiting mass for white-dwarf formation, but a value of 5 solar masses may be appropriate in a statistical sense for galactic model calculations.

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