Stellar evolution in the upper Hertzsprung-Russell diagram

Details Stellar evolution in the upper Hertzsprung-Russell diagram Stellar evolution in the upper Hertzsprung-Russell diagram

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...303..136d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 1, 1986, p. 136-145.

Statistics

Computation

44

Computational Astrophysics, Hertzsprung-Russell Diagram, Stellar Evolution, Supergiant Stars, Variable Stars, Wolf-Rayet Stars, Magnetohydrodynamic Stability, O Stars, Stellar Luminosity, Stellar Mass Ejection, Stellar Oscillations

Scientific paper

Evolutionary computations for massive stars, including mass loss and overshooting from convective cores, are presented. Using these computations, a coherent picture of the evolution of massive stars in the upper H-R diagram is given. Different formation mechanisms for various groups of luminous stars are discussed. Eta Carinae is interpreted as a very massive star suffering from a high mass loss, induced by vibrational instabilities. The Hubble-Sandage variables are divided into two groups: the more luminous ones are interpreted as Eta Carinae-like objects, while the less luminous ones are post-red supergiant stars. The boundary masses of progenitors of W-R systems formed through different scenarios are discussed. The observed ratio of W-R stars to O stars is discussed.

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