Main sequence for rotating stars of intermediate mass

Details Main sequence for rotating stars of intermediate mass Main sequence for rotating stars of intermediate mass

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.126...29e&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 126, no. 1, Oct. 1986, p. 29-50.

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11

Main Sequence Stars, Stellar Evolution, Stellar Mass, Stellar Rotation, Angular Velocity, Computational Astrophysics, Stellar Mass Ejection, Stellar Models

Scientific paper

The authors have investigated the evolutionary behaviour of intermediate mass (2, 3, 4, 5, and 7 M_sun;) Population I stars, assuming two different rates of rotation at the threshold of stability. In the first part of the study, stars are assumed to start with a critical rotation (fast rotation model) and to progress to the point of rotational instability. It is argued that multiple star systems might be formed through the evolution of rapidly rotating stars. In the second part of the study, stars are assumed to rotate at a rate below the critical value (slow rotation model). The evolutionary paths are found to be more or less similar to those of normal stars; but their positions on the main sequence are characterized by effective temperatures and luminosities lower than those of normal stars.

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