Spectral Types, Color Indices, and Abundances for Cepheids in the Magellanic Clouds and the Galaxy.

Details Spectral Types, Color Indices, and Abundances for Cepheids in the Magellanic Clouds and the Galaxy. Spectral Types, Color Indices, and Abundances for Cepheids in the Magellanic Clouds and the Galaxy.

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt........29l&link_type=abstract

Thesis (PH.D.)--BRIGHAM YOUNG UNIVERSITY, 1982.Source: Dissertation Abstracts International, Volume: 43-09, Section: B, page: 29

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Scientific paper

Accurate MK spectral types have been obtained for 58 Cepheids in the Galaxy and the Magellanic Clouds from 121 spectrograms. Simultaneous uvby(beta) photometry has been obtained with many of the spectrograms. The spectra of galactic and LMC Cepheids are found to be very similar, and Cepheids in both systems appear to obey the same (B -V)(,0) vs. spectral type relation. The low E(B-V) values of Feltz and McNamara (1980) and certain other recent authors are confirmed. The spectra of SMC Cepheids show slightly weaker metal lines, and SMC Cepheids average about 1.3 subclasses earlier in spectral type than LMC and galactic Cepheids at the same value of (B-V)(,0). Spectral types of LMC and SMC Cepheids at minimum light are found to be later than those reported by Feast (1974) when luminosity effects are allowed for. Curves of growth have been constructed for 7 SMC Cepheids, 5 LMC Cepheids, and 13 Milky Way Cepheids and spectral standards. Comparison indicates that Fe/H (,LMC) = -0.06 (+OR-) 0.10 and Fe/H(,SMC) = -0.50 (+OR-) 0.08.

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