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A Theoretical Period-Luminosity Relation of Dwarf Cepheids

Published online by Cambridge University Press:  12 April 2016

D.H. McNamara  and
John M. Powell
D.H. McNamara
Affiliation:
Department of Physics and AstronomyBrigham Young University Provo, Utah 84602USA
John M. Powell
Affiliation:
Department of Physics and AstronomyBrigham Young University Provo, Utah 84602USA

Extract

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Dwarf Cepheids (large-amplitude δ Sct variables and SXPhe variables in the GCVS) are late A-type stars near light maximum and early-F stars near light minimum. In the lower part of the instability strip where these stars are found the pulsation constant Q varies only slightly. As pointed out by Andreasen, Hejlesen, and Petersen (1983) this makes it easy to transform a theoretical HR or alternatively a (logTe, logg) diagram to a theoretical logTe, logP0) diagram by the use of the relation. This follows from the equations:

where P0 is the fundamental period of pulsation. The periods, of course, can be determined with very high accuracy.

Type
IV. Related Stars
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 437 - 438
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Andreasen, G.K., Hejlesen, P.M., and Petersen, J.O. 1983, A&A, 121, 241.Google Scholar
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