Eclipsing binaries with candidate CP stars. II. Parameters of the system V392 Carinae

Details Eclipsing binaries with candidate CP stars. II. Parameters of the system V392 Carinae Eclipsing binaries with candidate CP stars. II. Parameters of the system V392 Carinae

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...374..204d&link_type=abstract

Astronomy and Astrophysics, v.374, p.204-212 (2001)

Astronomy and Astrophysics

Astrophysics

10

Stars: Peculiar, Stars: Eclipsing Binaries, Stars: Spectroscopic Binaries

Scientific paper

We present a detailed study of an eclipsing binary which had been classified Ap SrCrEu (Hartoog \cite{hart}) before being known as a binary. Radial velocities measured at the times of both quadratures allow us to obtain precise masses for both components, while the light curve yields the radii. The following ephemeris and fundamental parameters of the system were obtained: HJD = (2447999.7656+/- 0.0041) + (3.174990+/-0.000001) E, e = 0.00, i = 81.9+/-0.1 deg, M1 = 1.90+/-0.02 Msun, M2 = 1.85 +/- 0.02 Msun, R1 = 1.63+/- 0.03 Rsun, R2 = 1.60+/- 0.03 Rsun, vsin i1 = 27.6+/-3.5 km s-1, vsin i2 = 23.6+/-3.6 km s-1. The projected rotational velocities were determined by fitting a synthetic spectrum convolved with a rotational profile to the observed spectrum. A comparison of the spectra of V392 Car and of the normal A star Cox 98, which has the same colour indices, shows that Sr is not overabundant and the metallicity of V392 Car is the same as that of the other cluster members. Therefore, V392 Car is a normal A2 star rather than an Ap star. The position of V392 Car in the HR diagram is entirely consistent with membership of the cluster NGC 2516. An independent estimate of the distance to this cluster was done using the parameters of the eclipsing system, and found to be in agreement with the Hipparcos one. A comparison of the parameters obtained from observations with predictions of internal structure models leads to a metallicity estimate [M/H]=0+/- 0.10 dex for NGC 2516. This estimate is completely independent of any spectroscopic or photometric method (except for the Teff determination) but relies on stellar structure models. Based on observations collected at the European Southern Observatory, La Silla, Chile (ESO programme No.~7-007, and Swiss 70~cm photometric telescope). Table 1 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/374/204

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