Supernova 1987A - the evolution from blue to red

Journal Article · Fri Sep 01 04:00:00 EDT 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/167849· OSTI ID:5357335

Tuchman, Y; Wheeler, J C ^[1]

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1. Texas Univ., Austin (USA)

The evolution of stars with mass comparable to that of the progenitor of SN 1987A from the main sequence to the Hayashi track is critically examined to determine why some models evolve to the red on nuclear time scales, some on thermal time scales, and some not at all. Thermal equilibrium solutions to a parametrized series of structural models with active hydrogen burning shells have two stable solutions with different T(eff) for the same helium core M(He) mass and a minimum M(He) below which no blue thermal equlibrium solution is possible. The dependence of the equilibrium solutions on stellar mass, envelope composition, and mass loss are investigated. The solutions quantitatively account for the 'gap' in the HR diagrams of massive stars in the Galaxy and LMC and suggest that the outer envelopes are not substantially enriched in helium during the first passage from the main sequence to the Hayashi track. 23 refs.

• OSTI ID: 5357335
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 344; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
DIAGRAMS
ELEMENTS
ERUPTIVE VARIABLE STARS
FLUIDS
GALAXIES
GASES
HELIUM
HERTZSPRUNG-RUSSELL DIAGRAM
HYDROGEN
HYDROGEN BURNING
MAGELLANIC CLOUDS
MAIN SEQUENCE STARS
MASS
MASS TRANSFER
MATHEMATICAL MODELS
NONMETALS
RARE GASES
STAR BURNING
STAR EVOLUTION
STAR MODELS
STARS
SUPERNOVAE
VARIABLE STARS