A simultaneous photometric and radial velocity study of short-period southern Cepheids. IV - Radii and masses

Details A simultaneous photometric and radial velocity study of short-period southern Cepheids. IV - Radii and masses A simultaneous photometric and radial velocity study of short-period southern Cepheids. IV - Radii and masses

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...260..208g&link_type=abstract

Astrophysical Journal, Part 1, vol. 260, Sept. 1, 1982, p. 208-219. Research supported by the Universidad de los Andes, and Fon

Astronomy and Astrophysics

Astrophysics

34

Astrometry, Cepheid Variables, Radial Velocity, Stellar Luminosity, Stellar Mass, Maximum Likelihood Estimates, Radii, Stellar Oscillations

Scientific paper

The maximum likelihood method of Balona (1977) is applied to simultaneous UBVRI(KC) photometric and photoelectric radial velocity observations of 15 southern Cepheids in order to derive the radii of the stars, and a new period-radius relationship for log P smaller than unity is constructed from these radii, whose slope agrees with Cogan's (1978) value of 0.70. Calculation and comparison of theoretical, pulsation and Wesselink radius masses of the Cepheids show basic agreement between theoretical and pulsation masses. A discrepancy persists between Wesselink radius masses and theoretical masses, the former being 20% smaller. The scatter of the Wesselink radius masses, however, is significantly reduced in comparison to Cox's results which do not suggest a need to invoke He-enriched surface layers in Cepheids. While the Wesselink radius mass discrepancy is slightly alleviated by the use of inhomogeneous models, agreement between theoretical and pulsation masses are better if the inhomogeneous model pulsation constant values are used.

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