Evolution of massive stars losing mass and angular momentum

Details Evolution of massive stars losing mass and angular momentum Evolution of massive stars losing mass and angular momentum

Dec 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....70..755s&link_type=abstract

Astronomy and Astrophysics, vol. 70, no. 6, Dec. 1978, p. 755-761. Research supported by the National Research Council of Canad

Astronomy and Astrophysics

Astrophysics

15

Angular Momentum, Stellar Evolution, Stellar Mass Ejection, Stellar Rotation, B Stars, Energy Conservation, Main Sequence Stars, Momentum Theory, Stellar Models, Variable Stars

Scientific paper

A phenomenological approach to incorporate the effect of rotation on the evolutionary pattern of massive mass-losing stars is taken on the basis of a 15-solar mass initial model at zero age. The mechanical equilibrium equation for a nonrotating model is modified by inclusion of the ratio of luminosity to Eddington luminosity and the ratio of the centrifugal force to the gravity force. It is assumed that the mass loss is proportional to the outward forces. Conservation statements then yield the equation for the spin-down rate of the star. Evolutionary tracks in the theoretical HR diagram are calculated for three sequences. If combined energy and angular momentum conservation is used, the models lose their spin in a time scale of order 5 million yr, starting from a rotational velocity above 500 km/sec, or 11.5 million years if only angular momentum conservation is used. Since the hydrogen burning lifetime of a 15-solar mass star is about 1.5 million years, it appears that rotational effects need not be considered for stars at this mass range in the subsequent evolutionary phases.

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