The Araucaria Project : the Baade-Wesselink projection factor of pulsating stars

Abstract

The projection factor used in the Baade-Wesselink methods of determining the distance of Cepheids makes the link between the stellar physics and the cosmological distance scale. A coherent picture of this physical quantity is now provided based on several approaches. We present the lastest news on the expected projection factor for different kinds of pulsating stars in the Hertzsprung-Russell diagram.

4 pages, 1 figure, Proceedings IAU Symposium No. 301, 2013

References in corpus (4)

• High resolution spectroscopy for Cepheids distance determination. I. Line asymmetry
• Physical parameters and the projection factor of the classical Cepheid in the binary system OGLE-LMC-CEP-0227
• Understanding the dynamical structure of pulsating stars: The center-of-mass velocity and the Baade-Wesselink projection factor of the beta-Cephei star alpha-Lupi
• Understanding the dynamical structure of pulsating stars: The Baade-Wesselink projection factor of the delta Scuti stars AI Vel and beta Cas

Cited by in corpus (5)

• Observational calibration of the projection factor of Cepheids - III. The long-period Galactic Cepheid RS Puppis
• HARPS-N high spectral resolution observations of Cepheids I. The Baade-Wesselink projection factor of δ Cep revisited
• Observational calibration of the projection factor of Cepheids I. The Type II Cepheid kappa Pavonis
• The long-period Galactic Cepheid RS Puppis - III. A geometric distance from HST polarimetric imaging of its light echoes
• Updated 24 $\mu \mathrm{m}$ Period-Luminosity Relation Derived from Galactic Cepheids