Bibcode
Huber, D.; Ireland, M. J.; Bedding, T. R.; Brandão, I. M.; Piau, L.; Maestro, V.; White, T. R.; Bruntt, H.; Casagrande, L.; Molenda-Żakowicz, J.; Silva Aguirre, V.; Sousa, S. G.; Barclay, T.; Burke, C. J.; Chaplin, W. J.; Christensen-Dalsgaard, J.; Cunha, M. S.; De Ridder, J.; Farrington, C. D.; Frasca, A.; García, R. A.; Gilliland, R. L.; Goldfinger, P. J.; Hekker, S.; Kawaler, S. D.; Kjeldsen, H.; McAlister, H. A.; Metcalfe, T. S.; Miglio, A.; Monteiro, M. J. P. F. G.; Pinsonneault, M. H.; Schaefer, G. H.; Stello, D.; Stumpe, M. C.; Sturmann, J.; Sturmann, L.; ten Brummelaar, T. A.; Thompson, M. J.; Turner, N.; Uytterhoeven, K.
Referencia bibliográfica
The Astrophysical Journal, Volume 760, Issue 1, article id. 32, 17pp, (2012).
Advertised on:
11
2012
Revista
Número de citas
189
Número de citas referidas
160
Descripción
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 = 4600-6200 K of –22
± 32 K (with a scatter of 97 K) and –58 ± 31 K (with
a scatter of 93 K), 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 HD 173701.
We conclude that the constraints presented in this study will have
strong potential for testing stellar model physics, in particular when
combined with detailed modeling of individual oscillation frequencies.
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