Fundamental properties of stars using asteroseismology from Kepler & CoRoT and interferometry from the CHARA Array

D. Huber, M. J. Ireland, T. R. Bedding, I. M. Brandão, L. Piau, V. Maestro, T. R. White, H. Bruntt, L. Casagrande, J. Molenda-Żakowicz, V. Silva Aguirre, S. G. Sousa, T. Barclay, C. J. Burke, W. J. Chaplin, J. Christensen-Dalsgaard, M. S. Cunha, J. De Ridder, C. Farrington, A. Frasca, R. A. García, R. L. Gilliland, P.J. Goldfinger, S. Hekker, S. D. Kawaler, H. Kjeldsen, H. McAlister, T. S. Metcalfe, A. Miglio, M. J. P. F. G. Monteiro, M. H. Pinsonneault, B. M. Schäfer, D. Stello, M. C. Stumpe, J. Sturmann, L. Sturmann, T. A. ten Brummelaar, M. J. Thompson, N. Turner, K. Uytterhoeven

Abstract
We present results of a long-baseline interferometry campaign using the PAVO beam combiner at the CHARA Array to measure the angular sizes of five main-sequence stars, one subgiant and four red giant stars for which solar-like oscillations have been detected by either Kepler or CoRoT. By combining interferometric angular diameters, Hipparcos parallaxes, asteroseismic densities, bolometric fluxes and high-resolution spectroscopy we derive a full set of near model-independent fundamental properties for the sample. We first use these properties to test asteroseismic scaling relations for the frequency of maximum power (νmax) and the large frequency separation (Δν). We find excellent agreement within the observational uncertainties, and empirically show that simple estimates of asteroseismic radii for main-sequence stars are accurate to ≲ 4%. We furthermore find good agreement of our measured effective temperatures with spectroscopic and photometric estimates with mean deviations for stars between T_eff = 4600 - 6200K of -22 ± 32K (with a scatter of 97K) and -58 ± 31K (with a scatter of 93K), respectively. Finally we present a first comparison with evolutionary models, and find differences between observed and theoretical properties for the metal-rich main-sequence star HD173701. We conclude that the constraints presented in this study will have strong potential for testing stellar model physics, in particular when combined with detailed modelling of individual oscillation frequencies.

Keywords
stars: late-type – stars: oscillations (including pulsations) – techniques: interferometric – techniques: photometric

The Astrophysical Journal
Volume 760, Page 32_1
November 2012

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