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Rotation and the Cepheid Mass Discrepancy

Published online by Cambridge University Press:  23 January 2015

Richard I. Anderson ,
Sylvia Ekström ,
Cyril Georgy ,
Georges Meynet ,
Nami Mowlavi  and
Laurent Eyer
Richard I. Anderson
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland email: [email protected]
Sylvia Ekström
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland email: [email protected]
Cyril Georgy
Affiliation:
Astrophysics group, Lennard-Jones Laboratories, EPSAM, Keele University, Staffordshire, ST5 5BG, UK
Georges Meynet
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland email: [email protected]
Nami Mowlavi
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland email: [email protected]
Laurent Eyer
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland email: [email protected]
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Abstract

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We recently showed that rotation significantly affects most observable Cepheid quantities, and that rotation, in combination with the evolutionary status of the star, can resolve the long-standing Cepheid mass discrepancy problem. We therefore provide a brief overview of our results regarding the problem of Cepheid masses. We also briefly mention the impact of rotation on the Cepheid period-luminosity(-color) relation, which is crucial for determining extragalactic distances, and thus for calibrating the Hubble constant.

Keywords

stars: evolutionstars: rotationsupergiantsCepheidsdistance scale
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 206 - 207
Copyright
Copyright © International Astronomical Union 2015 

References

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