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Spectrophotometry determination of Teff's for six Cepheids with P < 4 d

Published online by Cambridge University Press:  15 February 2018

E. Antonello ,
S. Fossati  and
L. Mantegazza
E. Antonello
Affiliation:
Osservatorio Astronomico di Brera, Merate, Italy
S. Fossati
Affiliation:
Dipartimento di Fisica, Università di Milano, Italy
L. Mantegazza
Affiliation:
Dipartimento di Fisica Nucleare e Teorica, Università di Pavia, Italy

Extract

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The population I Cepheids with 1.8 < P < 7 d are a non-homogeneous group in the sense that in this period range one can find fundamental, first overtone and double-mode pulsators. This implies that these three types of stars fall approximately in the same luminosity range. The knowledge of accurate physical parameters of these stars is therefore of paramount relevance in order to detect possible significant differences among different mode pulsators.

We have made spectrophotometric observations at La Silla Observatory of six Cepheids with P < 4 d (3 first-overtone and 3 fundamental mode pulsators). From a comparison with Kurucz's models of atmospheres (1979) we have derived their Teff's during the pulsational cycle. Due to the relevance of a correct estimate of the interstellar reddening in order to obtain accurate temperatures, we have independently determined the colour excesses of the studied objects by means of observations in the uvbyβ system using the method proposed by Feltz and McNamara (1980).

Type
Windows on the Instability Strip
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 377
Copyright
Copyright © Cambridge University Press 1993

References

Feltz, K.A., McNamara, D.H., 1980, Pub.Astr.Soc. Pacific, 92, 609.Google Scholar
Kurucz, R.L., 1979, Astrophys. J. Suppl., 40, 1.Google Scholar
Pel, J.W., 1978, Astron.Astrophys., 62, 75.Google Scholar
Teays, T.J., Schmidt, E.G., 1986, in: Stellar Pulsation, eds. Cox, A.N., Sparks, W.M. and Starrfield, S.G., Lecture Notes in Physics, p 173.Google Scholar