The mass of the classical Cepheid SU Cygni

Details The mass of the classical Cepheid SU Cygni The mass of the classical Cepheid SU Cygni

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...356..630e&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 20, 1990, p. 630-640. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

34

Binary Stars, Cepheid Variables, Stellar Mass, Stellar Oscillations, Ultraviolet Spectra, Center Of Mass, Hertzsprung-Russell Diagram, Main Sequence Stars, Stellar Mass Ejection

Scientific paper

Velocities of the companion of the classical Cepheid SU Cyg have been measured from 13 IUE high-dispersion spectra. Because the companion is itself a member of a short-period binary system, its short-period orbit and the orbital amplitude of the center of mass in the long-period system are determined from a triple system solution. The velocity amplitude of the short-period center of mass in the long-period orbit is 32.2 + or - 1.6 km/s. This leads to a mass ratio between the mass of the Cepheid and the sum of the masses of the companions of 1.07 + or - 0.05. Combining this mass ratio with the mass function from the Cepheid orbit produces a purely dynamical lower limit to the mass of the Cepheid of 5.9 + or - 0.4 solar masses, in good agreement with the evolutionary mass for the Cepheid without mass loss or convective overshoot near the main sequence.

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