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Absolute parameters for binary systems. I. The active binary BH Virginis
New high-quality light curves of the late-type binary system BH Vir havebeen obtained during a 6 year photometric uvby and H beta monitoringprogram of low mass eclipsing binaries (\cite[Clement et al.1997]{ref7}), hereafter Papers I and II. This paper presents detailedanalysis of this binary based on the four light curves obtained withinour program. The activity wave superimposed on the eclipse-modulatedlight curves has been adjusted and removed by using a new iterativeapplication of the standard EBOP code together with truncated FourierSeries fittings. Combining the recent radial velocity curves(\cite[Popper 1995]{ref23}) with the geometrical elements deduced fromthe "clean" photometric light curves, the absolute parameters of thesystem are calculated. BH Vir appears as a binary composed by two mainsequence G0 and G2 stars with solar chemical composition lying on thesame isochrone (log(tau)=9.8 +/- 0.2 years). The accuracy obtained onthe absolute parameters determination allows us to include BH Vir on theselect group of late-type stars to be used on the estimation of theMass-Luminosity-Relationship.
| Four colour photometry of late-type binary systems. II. New light curves of BH Virginis
This paper presents new complete uvby light curves of the late-typedetached eclipsing binary BH Vir (G0V + G5V, P=0.81687099 deg). Thisbinary system has been observed during four campaigns at the Calar AltoObservatory (Almeria, Spain) and at the European Southern Observatory(La Silla, Chile). This observations are part of a 6 year uvby andHβ monitoring program of low mass eclipsing binaries which mainobjective is to provide accurate absolute astrophysical parameters forlate-type main sequence stars. 1585 points spread over the binary periodand covering both eclipses are given. The internal accuracy of thestandard photometry measured as the mean RMS of the differences betweenstandard value and observed value for the standard stars observed alongthe program is quoted in a few millimagnitudes. Detailed analysis of BHVir, based on these light curves, will be published separately. Based onobservations collected with the Danish 0.5m telescope at the EuropeanSouthern Observatory (ESO), La Silla, Chile and the Spanish 1.5mtelescope at Calar Alto, Almeria, Spain. Table 2 will be accessible onlyin electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html.
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