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

By T. Boyajian, H. Mcalister, G. V. Belle, D. Gies, Theo., A. T. Brummelaar, K. von Braun, C. Farrington, P. J. Goldfinger, David and 10 more. 2011

137 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/cf1aace229839e1944e3e31d8bb7f27c51b5f3ee

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Huber
2. D. Stello
3. W. Chaplin
4. T. Bedding
5. A. Miglio
6. E. Gaidos
7. M. Pecaut
8. S. Hekker

In Instrumentation

1. D. Huber
2. D. Stello
3. W. Chaplin
4. T. Bedding
5. Eric Mamajek
6. S. Hekker
7. A. Miglio
8. Luca Casagrande

Citations in the corpus

• REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, methodology): “Finally, we checked all stars whose radii are measured with asteroseismic and interferometric methods (bottom panels in Figure 3, Boyajian et al. 2012, 2013; von Braun et al. 2014; Chaplin et al. 2014).”
• STELLAR DIAMETERS AND TEMPERATURES. II. MAIN-SEQUENCE K- AND M-STARS (2012, methodology): “The Astrophysical Journal, 757:112 (31pp), 2012 October 1 Boyajian et al. we fit flux-calibrated photometry to a Kurucz model spectral energy distribution (for details, see Boyajian et al. 2012).”
• STELLAR DIAMETERS AND TEMPERATURES. III. MAIN-SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS (2013, methodology): “The other measurements also include stars in DT1, DT2, and DT3 that have multiple measurements, and thus are not unique contributions to the ensemble of data (i.e., stars marked with a † in Table 3 and a † or †† in table 7 of DT2).”
• Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, background): “The latest generation of model spectra succeed in reproducing the broadband colors for FGK dwarfs and warm giants (Bertone et al. 2004, Kučinskas et al. 2005, Martins & Coelho 2007, Boyajian et al. 2012b).”
• INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, methodology): “We use photometry from Table 7 of Boyajian et al. (2012b), converting Johnson I to the Cousins system using the conversions in Bessell (1979) and converting Johnson JHK to the 2MASS system using the conversions of Carpenter (2001).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, background): “…in combination with a parallax, yields a linear radius and, when combined with an estimate for the bolometric flux, provides a direct measurement of a star’s effective temperature (see, e.g., Code et al. 1976; Boyajian et al. 2009; Baines et al. 2009; Boyajian et al. 2012a,b; Creevey et al. 2012).”