EDP Sciences
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Volume 428, Number 1, December II 2004
Page(s) 131 - 137
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20041419

A&A 428, 131-137 (2004)
DOI: 10.1051/0004-6361:20041419

Self consistent modelling of the projection factor for interferometric distance determination

N. Nardetto1, A. Fokin1, 2, 3, D. Mourard1, Ph. Mathias1, P. Kervella4 and D. Bersier5

1  Observatoire de la Côte d'Azur, Dpt. Gemini, UMR 6203, 06130 Grasse, France
    e-mail: Nicolas.Nardetto@obs-azur.fr
2  Institute of Astronomy of the Russian Academy of Sciences, 48 Pjatnitskaya Str., Moscow 109017, Russia
3  Isaak Newton Institute, Moscow Branch
4  Observatoire de Paris-Meudon, LESIA, UMR 8109, 5 place Jules Janssen, 92195 Meudon Cedex, France
5  Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

(Received 4 June 2004 / Accepted 28 July 2004 )

The distance of galactic Cepheids can be derived through the interferometric Baade-Wesselink method. The interferometric measurements lead to angular diameter estimations over the whole pulsation period, while the stellar radius variations can be deduced from the integration of the pulsation velocity. The latter is linked to the observational velocity deduced from line profiles by the so-called projection factor p. The knowledge of p is currently an important limiting factor for this method of distance determination. A self-consistent and time-dependent model of the star $\delta$ Cep is computed in order to study the dynamical structure of its atmosphere together with the induced line profile. Different kinds of radial and pulsation velocities are then derived. In particular, we compile a suitable average value for the projection factor related to different observational techniques, such as spectrometry, and spectral-line or wide-band interferometry. We show that the impact on the average projection factor and consequently on the final distance deduced from this method is of the order of 6%. We also study the impact of a constant or variable p-factor on the Cepheid distance determination. We conclude on this last point that if the average value of the projection factor is correct, then the influence of the time dependence is not significant as the error in the final distance is of the order of 0.2%.

Key words: stars: atmospheres -- stars: distances -- stars: oscillations -- stars: variables: Cepheids

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© ESO 2004