Interferometric radii of bright Kepler stars with the CHARA Array: θ Cygni and 16 Cygni A and B

被引：110

作者：

White, T. R. ^{[1
,2
,3
]}

Huber, D. ^{[1
,4
]}

Maestro, V. ^{[1
]}

Bedding, T. R. ^{[1
,3
]}

Ireland, M. J. ^{[1
,2
,5
]}

Baron, F. ^{[6
]}

Boyajian, T. S. ^{[7
,8
]}

Che, X. ^{[6
]}

Monnier, J. D. ^{[6
]}

Pope, B. J. S. ^{[1
]}

Roettenbacher, R. M. ^{[6
]}

Stello, D. ^{[1
,3
]}

Tuthill, P. G. ^{[1
]}

Farrington, C. D. ^{[7
]}

Goldfinger, P. J. ^{[7
]}

McAlister, H. A. ^{[7
]}

Schaefer, G. H. ^{[7
]}

Sturmann, J. ^{[7
]}

Sturmann, L. ^{[7
]}

ten Brummelaar, T. A. ^{[7
]}

Turner, N. H. ^{[7
]}

机构：

[1] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia

[2] Australian Astron Observ, Epping, NSW 1710, Australia

[3] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark

[4] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[5] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia

[6] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[7] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA

[8] Yale Univ, Dept Astron, New Haven, CT 06520 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2013年 / 433卷 / 02期

基金：

美国国家科学基金会; 新加坡国家研究基金会; 澳大利亚研究理事会;

关键词：

techniques: interferometric; stars: individual: theta Cygni; stars: individual: 16 Cygni A; stars: individual: 16 Cygni B; stars: oscillations; SOLAR-LIKE OSCILLATIONS; GENEVA-COPENHAGEN SURVEY; BASE-LINE INTERFEROMETRY; VIRTUAL OBSERVATORY TOOL; EXOPLANET HOST STARS; ANGULAR DIAMETERS; FUNDAMENTAL PROPERTIES; RED GIANTS; ULTRAVIOLET EXTINCTION; SEARCHING CALIBRATORS;

D O I：

10.1093/mnras/stt802

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the results of long-baseline optical interferometry observations using the Precision Astronomical Visual Observations (PAVO) beam combiner at the Center for High Angular Resolution Astronomy (CHARA) Array to measure the angular sizes of three bright Kepler stars: theta Cygni, and both components of the binary system 16 Cygni. Supporting infrared observations were made with the Michigan Infrared Combiner (MIRC) and Classic beam combiner, also at the CHARA Array. We find limb-darkened angular diameters of 0.753 +/- 0.009 mas for theta Cyg, 0.539 +/- 0.007 mas for 16 Cyg A and 0.490 +/- 0.006 mas for 16 Cyg B. The Kepler Mission has observed these stars with outstanding photometric precision, revealing the presence of solar-like oscillations. Due to the brightness of these stars the oscillations have exceptional signal-to-noise, allowing for detailed study through asteroseismology, and are well constrained by other observations. We have combined our interferometric diameters with Hipparcos parallaxes, spectrophotometric bolometric fluxes and the asteroseismic large frequency separation to measure linear radii (theta Cyg: 1.48 +/- 0.02 R-circle dot, 16 Cyg A: 1.22 +/- 0.02 R-circle dot, 16 Cyg B: 1.12 +/- 0.02 R-circle dot), effective temperatures (theta Cyg: 6749 +/- 44 K, 16 Cyg A: 5839 +/- 42 K, 16 Cyg B: 5809 +/- 39 K) and masses (theta Cyg: 1.37 +/- 0.04 M-circle dot, 16 Cyg A: 1.07 +/- 0.05 M-circle dot, 16 Cyg B: 1.05 +/- 0.04 M-circle dot) for each star with very little model dependence. The measurements presented here will provide strong constraints for future stellar modelling efforts.

引用

页码：1262 / 1270

页数：9

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