Mass loss in A and B supergiants and the extragalactic distance scale

Details Mass loss in A and B supergiants and the extragalactic distance scale Mass loss in A and B supergiants and the extragalactic distance scale

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...281...67t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 281, June 1, 1984, p. 67-75.

Astronomy and Astrophysics

Astrophysics

17

A Stars, B Stars, Early Stars, Magellanic Clouds, Stellar Mass Ejection, Supergiant Stars, Emission Spectra, H Alpha Line, H Beta Line, Metallicity, Stellar Luminosity, Stellar Spectra

Scientific paper

Samples of B5 and A0 stars in the Large Magellanic Cloud (LMC) demonstrate the existence of tight correlations between luminosity and equivalent widths in the H-alpha and H-beta lines. The H-alpha line is in emission for stars brighter than M(v) = -7, and this easily identifiable feature should be detectable at the distances of nearby groups of galaxies. The correlations imply that mass loss in A and B supergiants is strongly dependent on luminosity and therefore on stellar mass. Similar samples of stars in the Small Magellanic Cloud (SMC) shows systematically smaller H-alpha emission and more scatter in the relationships between luminosity and H-alpha line strengths than were found for the LMC stars. There is independent evidence that mass-loss rates are smaller in the SMC than in the LMC, and this fact probably accounts for the lower emission at H-alpha in the SMC stars. The differences between the samples in the two clouds may be caused by differences in stellar chemical composition.

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