Cepheid radii and masses from the surface-brightness method

Details Cepheid radii and masses from the surface-brightness method Cepheid radii and masses from the surface-brightness method

Sep 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.222..251g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 222, Sept. 15, 1986, p. 251-260. Research supported by

Astronomy and Astrophysics

Astronomy

13

Brightness Distribution, Cepheid Variables, Mass To Light Ratios, Surface Properties, Milky Way Galaxy, Radial Velocity, Radii, Star Distribution, Stellar Color, Stellar Spectrophotometry, Ubv Spectra

Scientific paper

Simultaneous photometric BVRI and radial velocity data on classical Cepheids, including long-period stars, are used to obtain a more significant period-radius relationship from the surface-brightness technique of Barnes and Evans (1976). The resulting period-radius relationship agrees well with the one derived from the luminosities and effective temperatures of the cluster and association Cepheids if the fainter Cepheid luminosities advocated by Schmidt (1984), Boehm-Vitense (1985), and Gieren (1986) are used instead of the luminosity scale of Fernie and McGonegal (1983). The surface brightness results support the view that the correct slope of the period-radius relation is between 0.75 and 0.80.

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