The masses of AC Andromedae, U Trianguli Australis, and BC Draconis

Details The masses of AC Andromedae, U Trianguli Australis, and BC Draconis The masses of AC Andromedae, U Trianguli Australis, and BC Draconis

Mar 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...212..451c&link_type=abstract

Astrophysical Journal, Part 1, vol. 212, Mar. 1, 1977, p. 451-458. ERDA-sponsored research

Astronomy and Astrophysics

Astrophysics

21

Cepheid Variables, Pulsed Radiation, Stellar Luminosity, Stellar Mass, Radii, Stellar Evolution, Stellar Models, Stellar Temperature

Scientific paper

Special calculations in the framework of linear radial-pulsation theory are performed to derive masses that closely match the observed periods of the double-mode variables AC And, U TrA, and BC Dra. Purely radiative models are constructed for varying mass, effective temperature, luminosity, and composition, with the effective-temperature range corresponding to the observed pulsational-instability strip. A number of models which include 'frozen-in' convection in the mixing-length approximation are also considered, and several models are computed at effective-temperature values near the red edge of the instability strip. The results indicate that AC And may be a high-luminosity Delta Scuti star since its mass is too large for an ordinary RR Lyrae star, that U TrA must be cooler than 6400 K, and that the temperature of BC Dra cannot be higher than about 5700 K to have a second-order pulsational instability in terms of the linear theory. It is noted that the derived mass of BC Dra is only seven-tenths that given by stellar evolution theory.

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