M supergiants and the low metal abundances in the Small Magellanic Cloud

Details M supergiants and the low metal abundances in the Small Magellanic Cloud M supergiants and the low metal abundances in the Small Magellanic Cloud

Jul 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...231..384h&link_type=abstract

Astrophysical Journal, Part 1, vol. 231, July 15, 1979, p. 384-387.

Astronomy and Astrophysics

Astrophysics

53

Abundance, Late Stars, M Stars, Magellanic Clouds, Supergiant Stars, Astronomical Photometry, Atmospheric Composition, Electrophotometry, Metals, Stellar Atmospheres

Scientific paper

BVRI photometry of 25 spectroscopically confirmed M supergiants in the Small Magellanic Cloud (SMC) is discussed. It is found that one of these stars is of spectral type M1 and that the rest have spectral types M0 or earlier. Two-color plots are presented which show that only one M supergiant in the SMC may be as late as M2. It is suggested that lower metallicities in the SMC may produce lower opacities in the atmospheres of cool supergiants, so that the spectra originate in somewhat warmer layers and give rise to earlier spectral types.

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