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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.
| A photometric study of NN Virginis
Photoelectric BV light curves of the recently discovered eclipsingbinary NN Vir were studied for the first time to derive the physicalparameters of the system. The light curves were obtained at the AnkaraUniversity Observatory during three nights in May, 2002. The solutionsmade by using Djurasevic's inverse problem method describe the NN Virsystem as a high overcontact configuration (f_over 58%) with arelatively small temperature differences between the components (ΔT=Th-Tc 160 K). These solutions suggest asignificant mass and energy transfer from the more massive primary ontothe less massive secondary. The hot area on the less massive star, nearthe neck region, can be taken as a consequence of this mass and energyexchange between the components through the connecting neck of thecommon envelope.Table 2 is only available in electronic form at CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/415/283
| Photoelectric Minima of Some Eclipsing Binary Stars
We present 21 minima times of 7 eclipsing binaries made in the years of2001 and 2002.
| Interstellar polarization from observations of A and F stars in high and intermediate galactic latitudes, and from stars in the Mathewson and Ford polarization catalogue
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1986A&AS...64..487K&db_key=AST
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| Takýmyýldýz: | Basakci |
| Sað Açýklýk: | 14h16m34.76s |
| Yükselim: | +05°31'55.2" |
| Görünürdeki Parlaklýk: | 8.332 |
| Uzaklýk: | 139.47 parsek |
| özdevim Sað Açýklýk: | -0.7 |
| özdevim Yükselim: | 3.5 |
| B-T magnitude: | 8.838 |
| V-T magnitude: | 8.374 |
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