• DOI:10.1088/0004-637X/746/1/101
• Corpus ID: 18993744

STELLAR DIAMETERS AND TEMPERATURES. I. MAIN-SEQUENCE A, F, AND G STARS

@article{Boyajian2012STELLARDA,
  title={STELLAR DIAMETERS AND TEMPERATURES. I. MAIN-SEQUENCE A, F, AND G STARS},
  author={Tabetha S. Boyajian and Harold A. Mcalister and Gerard T. van Belle and Douglas R. Gies and Theo A. ten Brummelaar and Kaspar von Braun and Christopher D. Farrington and P. J. Goldfinger and David P. O'Brien and J. Robert Parks and Noel D. Richardson and Stephen T. Ridgway and Gail H. Schaefer and Laszlo Sturmann and Judit Sturmann and Yamina Touhami and Nils H. Turner and Russel J. White},
  journal={The Astrophysical Journal},
  year={2012},
  volume={746}
}

• T. Boyajian, H. Mcalister, +15 authors R. White
• Published 14 December 2011
• Physics
• The Astrophysical Journal

We have executed a survey of nearby, main-sequence A-, F-, and G-type stars with the CHARA Array, successfully measuring the angular diameters of forty-four stars with an average precision of ∼1.5%. We present new measures of the bolometric flux, which in turn leads to an empirical determination of the effective temperature for the stars observed. In addition, these CHARA-determined temperatures, radii, and luminosities are fit to Yonsei–Yale model isochrones to constrain the masses and ages of the stars. These results are compared to indirect estimates of these quantities obtained by collecting photometry of the stars and applying them to model atmospheres and evolutionary isochrones. We find that for most cases, the models overestimate the effective temperature by ∼1.5%–4% when compared to our directly measured values. The overestimated temperatures and underestimated radii in these works appear to cause an additional offset in the star's surface gravity measurements, which consequently yield higher masses and younger ages, in particular for stars with masses greater than ∼1.3 M☉. Additionally, we compare our measurements to a large sample of eclipsing binary stars, and excellent agreement is seen within both data sets. Finally, we present temperature relations with respect to (B − V) and (V − K) colors as well as spectral type, showing that calibration of effective temperatures with errors ∼1% is now possible from interferometric angular diameters of stars.