No CrossRef data available.
Article contents
A Theoretical Period-Luminosity Relation of Dwarf Cepheids
Published online by Cambridge University Press: 12 April 2016
Extract
Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.
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
- Copyright
- Copyright © Astronomical Society of the Pacific 1993
References
Mengel, J.G., Sweigart, A.V., DeMarque, P., and Gross, P.G.
1979, APJS, 40, 733.CrossRefGoogle Scholar
Nemec, J., and Mateo, M.
1990 in Confrontation Between Stellar Pulsation and Evolution, eds. Cacciari, C. and Clementini, G., ASPCONF SER
11, 64.Google Scholar
You have
Access