Large Magellanic Cloud helium-rich peculiar blue supergiants and SN 1987A

Details Large Magellanic Cloud helium-rich peculiar blue supergiants and SN 1987A Large Magellanic Cloud helium-rich peculiar blue supergiants and SN 1987A

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...363..255t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 363, Nov. 1, 1990, p. 255-264. Research supported by the University of Texa

Astronomy and Astrophysics

Astrophysics

28

Blue Stars, Magellanic Clouds, Peculiar Stars, Star Distribution, Supergiant Stars, Supernova 1987A, Helium, Hertzsprung-Russell Diagram, Stellar Envelopes, Stellar Evolution, Stellar Mass

Scientific paper

The theoretical distribution of massive stars in the H-R diagram is compared to the revised data of Fitzpatrick and Garmany for the LMC. Preferred models of about 20 M solar masses undergo a thermal contraction at T(eff) about 35,000 K at the end of core hydrogen burning but reestablish thermal equilibrium to the red of the main sequence at T(eff) about 20,000 K after ignition of a hydrogen-burning shell. They then evolve on a nuclear time scale to T(eff) about 6000 K where they lose thermal equilibrium and jump to the Hayashi track. The theoretical and observed distributions agree with two significant exceptions: the blue thermal contraction 'gap' is overpopulated compared to the theory, and there is a 'ledge' crossing the center of the H-R diagram. The hypothesis that some of the observed stars int he blue 'gap' are secondaries that have accreted helium-rich matter from deep within the hydrogen envelope of a red supergiant primary is explored. some preliminary observational justification is given.

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