Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...331..388s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 331, Aug. 1, 1988, p. 388-393.
Astronomy and Astrophysics
Astrophysics
67
Blue Stars, Red Giant Stars, Stellar Envelopes, Stellar Evolution, Stellar Interiors, Supernova 1987A, Hydrogen, Light Curve, Stellar Composition, Stellar Mass Ejection, Stellar Models
Scientific paper
Systematic evolutionary calculations for a star with an initial mass of 20 solar masses have been performed to clarify the way in which evolutionary path depends on mass loss, metallicity, and helium abundances and under what conditions a star like the progenitor of SN 1987A undergoes a blue-red-blue evolution. It is found that the star evolves from the blue to the red when the mass of the hydrogen-rich envelope significantly decreases, and comes back from the red to the blue before carbon ignition if the helium abundance is sufficiently enhanced by mass loss and mixing. For lower metallicity, such an evolution occurs for a wider range of parameter space. Although the mass loss is important, the progenitor can retain a hydrogen-rich envelope of 5-10 solar masses.
Kato Mariko
Nomoto Ken'ichi
Saio Hideyuki
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