The energy distributions of B supergiants in the Large Magellanic Cloud

Details The energy distributions of B supergiants in the Large Magellanic Cloud The energy distributions of B supergiants in the Large Magellanic Cloud

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986esasp.263..423f&link_type=abstract

In ESA Proceedings of an International Symposium on New Insights in Astrophysics. Eight Years of UV Astronomy with IUE p 423-42

Astronomy and Astrophysics

Astrophysics

1

Magellanic Clouds, Spectral Energy Distribution, Stellar Atmospheres, Stellar Models, Stellar Spectra, Supergiant Stars, Stellar Evolution, Stellar Gravitation, Stellar Luminosity, Stellar Temperature

Scientific paper

It is shown that line-blanketed, LTE, plane-parallel model atmosphere calculations provide excellent fits to the ultraviolet-through-visual energy distributions of B supergiants in the Large Magellanic Cloud. The models were computed using Kurucz's (1979) ATLAS atmosphere program, but with lower gravities than were contained in Kurucz's published model grid. The ultraviolet continua of low gravity stars are found to be sensitive to changes in temperature and gravity. Measurements of Teff and log g for ten LMC B supergiants from model atmosphere fits to the energy distributions yield estimates of their radii, luminosities, and masses. Model atmosphere fits suggest that the late B supergiants have significantly lower masses than the earlier B types of the same luminosity, contrary to stellar evolution theory which predicts that B supergiants are in a post-core hydrogen burning phase and should evolve very quickly and at essentially constant mass.

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