Physical parameters and pulsational mode of short-period small-amplitude Cepheids

Details Physical parameters and pulsational mode of short-period small-amplitude Cepheids Physical parameters and pulsational mode of short-period small-amplitude Cepheids

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.209..481a&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 209, Aug. 1, 1984, p. 481-502. Research supported by th

Astronomy and Astrophysics

Astronomy

45

Cepheid Variables, Stellar Oscillations, Supergiant Stars, Vibration Mode, H Alpha Line, Stellar Luminosity, Stellar Mass, Stellar Temperature

Scientific paper

Nine galactic short-period (P less than 8 days) small-amplitude Cepheids have been the subject of a study to determine their physical parameters and pulsational properties. UBVRI photometry and radial velocities were obtained in the same observing seasons. The wings of H-alpha were used to determine effective temperatures. Empirical radii, luminosities, and masses were determined. The short-period stars lie inside and seem to be on the red side of the observational Cepheid instability strip. It was found that these stars are likely pulsating in the radial fundamental mode except HR 8084 (DT Cyg) which is suspected to be a first overtone pulsator. As the small-amplitude Cepheids in the LMC are thought to be first overtone pulsators, it is suggested that small-amplitude sinusoidal variations are not the consequence of pulsation in the first overtone, but rather the response to a more general amplitude trend across the instability strip in a particular galactic system.

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