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The empirical period-radius relation for pulsating stars: a synthesis based on photometric and radial velocity measurements
Published online by Cambridge University Press: 04 August 2017
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The relation existing between the radius and the period for the pulsating stars of a given class constitutes a powerful test for the theory of stellar evolution and for the identification of the pulsation modes. In recent years, several authors have determined the mean radius of a lot of pulsating stars of various classes by applying the Baade-Wesselink method. Fig. 1 presents the resulting general logP - logR diagram grouping these determinations. The sources for the radii are given by Burki and Meylan (1986). The variable stars in known binaries have been excluded since the presence of a companion biases the radius calculation (Burki, 1984). The determinations marked by arrows are based on the radial velocities by CORAVEL (1m telescope at the Haute-Provence Observatory, France) or/and on the photometry in the Geneva system (40cm and 70cm telescopes at La Silla Observatory, Chile).
- Type
- II. Photometric Research Programmes
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- Copyright © Reidel 1986
References
Burki, G.: 1985, Duplicity, Mass Loss and the Cepheid Mass Anomaly, in Cepheids: Observations and Theory, IAU Coll. no 82, Ed. Madore, B.F., Cambridge Univ. Press, Cambridge, p. 71
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Harris, H.: 1985, Population II Cepheids, in Cepheids: Observations and Theory, IAU Coll. no 82, Ed. Madore, B.F., Cambridge Univ. Press, Cambridge, p. 232
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