Appourchaux, T. and Antia, H. M. and Ball, W. and Creevey, O. and Lebreton, Y. and Verma, K. and Vorontsov, S. and Campante, T. L. and Davies, G. R. and Gaulme, P. and Regulo, C. and Horch, E. and Howell, S. and Everett, M. and Ciardi, D. and Fossati, L. and Miglio, A. and Montalban, J. and Chaplin, W. J. and Garcia, R. A. and Gizon, L. (2015) A seismic and gravitationally bound double star observed by Kepler: implication for the presence of a convective core. Astronomy and Astrophysics, 582. pp. 119. ISSN 00046361

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Abstract
Context. Solarlike oscillations have been observed by Kepler and CoRoT in many solartype stars, thereby providing a way to probe stars using asteroseismology. Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a doublestar system (HIP93511), for which an interferometric orbit has been observed along with asteroseismic measurements. Methods. We used a time series of nearly two years of data for the double star to detect the two oscillationmode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system. Results. From the determination of the orbit, the total mass of the system is 2.34<inf>0.33</inf><sup>+0.45</sup> M<inf>⊙</inf>. The total seismic mass using scaling relations is 2.47 ± 0.07 M<inf>⊙</inf>. The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.73.9 Gyr. The mean total seismic mass of the system is 2.342.53 M<inf>⊙</inf> consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as R<inf>A</inf> = 1.821.87R<inf>⊙</inf>, M<inf>A</inf> = 1.251.39 M<inf>⊙</inf>, Age<inf>A</inf> = 2.63.5 Gyr; R<inf>B</inf> = 1.221.25 R<inf>⊙</inf>, M<inf>B</inf> = 1.081.14 M<inf>⊙</inf>, Age<inf>B</inf> = 3.354.21 Gyr. The models provide two sets of values for Star A: [1.251.27] M<inf>⊙</inf> and [1.341.39] M<inf>⊙</inf>. We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.141.25] M<inf>⊙</inf>.
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Item Type:  Article (Commonwealth Reporting Category C) 

Refereed:  Yes 
Item Status:  Live Archive 
Additional Information:  Access to published version in accordance with the copyright policy of the publisher. 
Faculty / Department / School:  No Faculty 
Date Deposited:  14 Jun 2017 04:04 
Last Modified:  14 Jun 2017 04:04 
Uncontrolled Keywords:  asteroseismology; astrometry; binaries: general; stars: evolution; solartype stars; Earthquake Measurements and Analysis; Extraterrestrial Physics and Stellar Phenomena; Storage; Light and Optics; Chemical Operations; Optical Variables Measurements; 
Fields of Research :  02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems 
SocioEconomic Objective:  E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences 
Identification Number or DOI:  10.1051/00046361/201526610 
URI:  http://eprints.usq.edu.au/id/eprint/32101 
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