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Four-colour photometry of eclipsing binaries. XLI.. uvby light curves for AD Bootis, HW Canis Majoris, SW Canis Majoris, VZ Hydrae, and WZ Ophiuchi
Context: Accurate mass, radius, and abundance determinations frombinaries provide important information on stellar evolution, fundamentalto central fields in modern astrophysics and cosmology. Aims:Within the long-term Copenhagen Binary Project, we aim to obtainhigh-quality light curves and standard photometry for double-lineddetached eclipsing binaries with late A, F, and G type main-sequencecomponents, needed for the determination of accurate absolute dimensionsand abundances, and for detailed comparisons with results from recentstellar evolutionary models. Methods: Between March 1985 and July2007, we carried out photometric observations of AD Boo, HW CMa, SW CMa,V636 Cen, VZ Hya, and WZ Oph at the Strömgren Automatic Telescopeat ESO, La Silla. Results: We obtained complete {uvby} lightcurves, ephemerides, and standard {uvby}? indices for all sixsystems. For V636 Cen and HW CMa, we present the first modern lightcurves, whereas for AD Boo, SW CMa, VZ Hya, and WZ Oph, they are bothmore accurate and more complete than earlier data. Due to a high orbitaleccentricity (e = 0.50), combined with a low orbital inclination (i =84.7°), only one eclipse, close to periastron, occurs for HW CMa.For the two other eccentric systems, V636 Cen (e = 0.134) and SW CMa (e= 0.316), apsidal motion has been detected with periods of 5270 ±335 and 14 900 ± 3600 years, respectively.Based on observations carried out with the Strömgren AutomaticTelescope (SAT) at ESO, La Silla, Chile. Appendix A is only available inelectronic form at http://www.aanda.org Tables 6-13 are only availablein electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr(130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/487/1081
| Effective temperature scale and bolometric corrections from 2MASS photometry
We present a method to determine effective temperatures, angularsemi-diameters and bolometric corrections for population I and II FGKtype stars based on V and 2MASS IR photometry. Accurate calibration isaccomplished by using a sample of solar analogues, whose averagetemperature is assumed to be equal to the solar effective temperature of5777 K. By taking into account all possible sources of error we estimateassociated uncertainties to better than 1% in effective temperature andin the range 1.0-2.5% in angular semi-diameter for unreddened stars.Comparison of our new temperatures with other determinations extractedfrom the literature indicates, in general, remarkably good agreement.These results suggest that the effective temperaure scale of FGK starsis currently established with an accuracy better than 0.5%-1%. Theapplication of the method to a sample of 10 999 dwarfs in the Hipparcoscatalogue allows us to define temperature and bolometric correction (Kband) calibrations as a function of (V-K), [m/H] and log g. Bolometriccorrections in the V and K bands as a function of T_eff, [m/H] and log gare also given. We provide effective temperatures, angularsemi-diameters, radii and bolometric corrections in the V and K bandsfor the 10 999 FGK stars in our sample with the correspondinguncertainties.
| UvbyHbeta_ photometry of main sequence A type stars.
We present Stroemgren uvby and Hbeta_ photometry for a set of575 northern main sequence A type stars, most of them belonging to theHipparcos Input Catalogue, with V from 5mag to 10mag and with knownradial velocities. These observations enlarge the catalogue we began tocompile some years ago to more than 1500 stars. Our catalogue includeskinematic and astrophysical data for each star. Our future goal is toperform an accurate analysis of the kinematical behaviour of these starsin the solar neighbourhood.
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| Takýmyýldýz: | Su Yilani |
| Sað Açýklýk: | 08h34m37.63s |
| Yükselim: | -02°45'16.4" |
| Görünürdeki Parlaklýk: | 7.614 |
| Uzaklýk: | 165.017 parsek |
| özdevim Sað Açýklýk: | -14.5 |
| özdevim Yükselim: | -10.1 |
| B-T magnitude: | 7.851 |
| V-T magnitude: | 7.634 |
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