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Fourier analysis of Beat Cepheids

Published online by Cambridge University Press:  25 April 2016

D. J. Faulkner
D. J. Faulkner*
Affiliation:
Mount Stromlo and Siding Spring Observatory, Australian National University
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Extract

The double-mode or beat Cepheids form a group of some 10 variables at the short period end of the classical Cepheid period range, which exhibit two (or three) simultaneous pulsations with remarkably constant period ratio (see Table I). If, as seems likely, the two periods (P0 and P1,) are to be identified with fundamental and first-overtone radial oscillations, linear pulsation theory may be used to yield a mass and a radius estimate for each beat Cepheid (Mbear and Rbeat) based on period observations alone. The masses so obtained may be compared with two other Cepheid mass estimates: the pulsation mass, Mpuls, is derived by the application of pulsation theory to one observed stellar period (usually P0) and a radius calculated from the stellar luminosity and temperature; the evolutionary mass, Mevol, is inferred from the stellar luminosity by the application of stellar evolution results (without mass loss) for Population I stars in the core helium-burning phase. If a Cepheid is a member of a cluster or association whose distance and reddening have been determined, the Cepheid luminosity and temperature may be obtained observationally, yielding Mpuls, and Mevol estimates directly. For other Cepheids, only indirect estimates may be made, based on the period-luminosity-colour relationship calibrated using the Cepheids with cluster membership.

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Publications of the Astronomical Society of Australia , Volume 3 , Issue 2 , September 1977 , pp. 124 - 128
Copyright
Copyright © Astronomical Society of Australia 1977

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