J/MNRAS/363/529ivo://CDS.VizieR/J/MNRAS/363/529doi:10.26093/cds/vizier.73630529CDSSouthworth J.Smalley B.Maxted P.F.L.Claret A.Etzel P.B.2024-07-01T20:15:24Z2008-02-27T13:50:09ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.freclipsing-binary-starsvisible-astronomymedium-band-photometrybroad-band-photometryradial-velocityWW Aurigae is a detached eclipsing binary composed of two metallic- lined A-type stars orbiting each other every 2.5 days. We have determined the masses and radii of both components to accuracies of 0.4% and 0.6%, respectively. From a cross-correlation analysis of high-resolution spectra we find masses of 1.964+/-0.007M_{sun}_ for the primary star and 1.814+/-0.007M_{sun}_ for the secondary star. From an analysis of photoelectric uvby and UBV light curves we find the radii of the stars to be 1.927+/-0.011R_{sun}_ and 1.841+/-0.011R_{sun}_, where the uncertainties have been calculated using a Monte Carlo algorithm. Fundamental effective temperatures of the two stars have been derived, using the Hipparcos parallax of WW Aur and published ultraviolet, optical and infrared fluxes, and are 7960+/-420 and 7670+/-410K. The masses, radii and effective temperatures of WW Aur are only matched by theoretical evolutionary models for a fractional initial metal abundance, Z, of approximately 0.06 and an age of roughly 90Myr. This seems to be the highest metal abundance inferred for a well-studied detached eclipsing binary, but we find no evidence that it is related to the metallic-lined nature of the stars. The circular orbit of WW Aur is in conflict with the circularization timescales of both the Tassoul and the Zahn tidal theories and we suggest that this is due to pre-main-sequence evolution or the presence of a circular orbit when the stars were formed.2005MNRAS.363..529Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/363/529CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/363/529https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/363/529http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/363/529https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/363/529https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/363/529http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/363/529GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/MNRAS/363/529/minimaTimes of minimum light from the literaturerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian Date times of minimum lightdtime.epochdoubleJ/MNRAS/363/529/photPhotometric data (merging of the individual tables)HJDHJD of observationdtime.epoch;obsdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBand[uvbyUBV] Photometric bandinstr.bandpasschardmagObserved differential magnitudemagphot.mag;arith.diffdoubleJ/MNRAS/363/529/rvRadial velocities of both components of WW Aur (Kiyokawa & Kitamura, 1975AnTok..15..117K)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHJD of observationdtime.epoch;obsdoubleRV(A)Measured radial velocity of primary starkm/sphys.veloc;pos.heliocentricfloatRV(B)Measured radial velocity of secondary starkm/sphys.veloc;pos.heliocentricfloat