FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM<i>KEPLER</i>AND<i>CoRoT</i>AND INTERFEROMETRY FROM THE CHARA ARRAY

Huber, Daniel; Ireland, Michael; Bedding, Timothy R.; Brandão, I. M.; Piau, L.; Maestro, Vicente; White, T. R.; Bruntt, H.; Casagrande, Luca; Molenda-Żakowicz, J.; Aguirre, V. Silva; Sousa, S. G.; Barclay, Thomas; Burke, Christopher J.; Chaplin, W. J.; Christensen‐Dalsgaard, J.; Cunha, M. S.; Ridder, J. De; Farrington, C.; Frasca, A.; García, R. A.; Gilliland, Ronald L.; Goldfinger, P. J.; Hekker, S.; Kawaler, S. D.; Kjeldsen, H.; McAlister, Harold A.; Metcalfe, T. S.; Miglio, A.; Monteiro, M. J. P. F. G.; Pinsonneault, Marc H.; Schaefer, Gail H.; Stello, Dennis; Stumpe, Martin C.; Sturmann, J.; Sturmann, L.; Brummelaar, Theo A. ten; Thompson, M. J.; Turner, N.; Uytterhoeven, K.

doi:10.1088/0004-637x/760/1/32

Cited by 224 publications

(179 citation statements)

References 148 publications

(237 reference statements)

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“…The proper calibration of stellar radii can be performed by using stellar radii derived using interferometric measurements (Creevey et al 2007;Bigot et al 2011;Bazot et al 2011;Huber et al 2012;White et al 2013). With these interferometric stellar radii, one can also derive a proxy of the stellar masses using scaling relations as in Huber et al (2012), stellar masses that also need an independent calibration.…”

Section: Introductionmentioning

confidence: 99%

“…With these interferometric stellar radii, one can also derive a proxy of the stellar masses using scaling relations as in Huber et al (2012), stellar masses that also need an independent calibration. The best way to measure stellar masses is to use binary systems for which the orbital motion can be observed either by spectroscopy or by imagery.…”

Section: Introductionmentioning

confidence: 99%

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A seismic and gravitationally bound double star observed byKepler

Appourchaux

Antia

Ball

et al. 2015

A&A

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Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type 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 double-star system (HIP 93511), 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 oscillation-mode 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 +0.45 −0.33 M . The total seismic mass using scaling relations is 2.47 ± 0.07 M . 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 2.7-3.9 Gyr. The mean total seismic mass of the system is 2.34-2.53 M consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as R A = 1.82−1.87 R , M A = 1.25−1.39 M , Age A = 2.6-3.5 Gyr; R B = 1.22−1.25 R , M B = 1.08−1.14 M , Age B = 3.35-4.21 Gyr. The models provide two sets of values for Star A: [1.25-1.27] M and [1.34-1.39] M . 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 [1.14-1.25] M .

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A seismic and gravitationally bound double star observed byKepler

Appourchaux

Antia

Ball

et al. 2015

A&A

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“…1 and 2 that when these data are available, a direct estimation of the stellar mass and radius can be obtained (e.g., Silva Aguirre et al 2011;Stello et al 2008). These scaling relations seem to hold well for radius determinations (e.g., Huber et al 2012;North et al 2007;Silva Aguirre et al 2012;White et al 2013), while confirmation of masses is still under way using clusters and binaries. In order to determine ages for stars using the global seismic parameters, BASTA and BeSPP compare these quantities and the atmospheric parameters to those predicted by grids of models.…”

Section: The Bare Minimummentioning

confidence: 82%

Asteroseismic age determination for dwarfs and giants

Aguirre

Serenelli

2016

Astron Nachr

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Asteroseismology can make a substantial contribution to our understanding of the formation history and evolution of our Galaxy by providing precisely determined stellar properties for thousands of stars in different regions of the Milky Way. We present here the different sets of observables used in determining asteroseismic stellar properties, the typical level of precision obtained, the current status of results for ages of dwarfs and giants and the improvements than can be expected in the near future in the context of Galactic archaeology.

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“…Mortier et al (2013b) discuss the impact that different methods of surface gravity estimation can have on the determination of stellar masses. In a similar way, Huber et al (2012) compare asteroseismic surface gravities with those obtained from the analysis of photometric light curves. Method 2-Use of the Torres et al (2010) empirical relation between stellar mass, effective temperature, surface gravity and metal abundance, derived from the analysis of stellar binaries:…”

Section: O B S E Rvat I O Na L Data a N D M E T H O D O L O G Ymentioning

confidence: 99%

“…This technique can result in mass uncertainties below 5 per cent if a few frequencies with an uncertainty below 0.1 µHz are available (e.g. Kjeldsen, Bedding & Christensen-Dalsgaard 2009;Huber et al 2012;Mathur et al 2012;Creevey et al 2013;Chaplin et al 2014 and references therein). The main drawback for this is the fact that the number of stars that fulfil the above precision in frequencies is still small.…”

Section: Introductionmentioning

confidence: 99%

On the mass estimation for FGK stars: comparison of several methods

Pinheiro

Fernandes

Cunha

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Stellar evolutionary models simulate well binary stars when individual stellar mass and system metallicity are known. The mass can be derived directly from observations only in the case of multiple stellar systems, mainly binaries. Yet, the number of such stars for which accurate stellar masses are available is rather small. The main goal of this project is to provide realistic mass estimates for a homogeneous sample of about a thousand FGK single stars, using four different methods and techniques. We present the masses inferred according to each one of these methods as well as a final mass estimate consisting in the median of the four mass estimates. The procedures evaluated here include the use of stellar evolutionary models, massluminosity relation and surface gravity spectroscopic observations. By combining the results obtained with different methods, we determine the best mass value for each individual star, as well as the associated error budget. Our results confirm the expected consistency between the different mass estimation methods. None the less, for masses above 1.2 M , the spectroscopic surface gravities seem to overestimate the mass. This result may be a consequence of the spectroscopic surface gravities used in this analysis. Nevertheless, this problem is minimized by the fact that we have several approaches available for deriving stellar masses. Moreover, we suggest an empirical procedure to overcome this issue.

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FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROMKEPLERANDCoRoTAND INTERFEROMETRY FROM THE CHARA ARRAY

Cited by 224 publications

References 148 publications

A seismic and gravitationally bound double star observed byKepler

A seismic and gravitationally bound double star observed byKepler

Asteroseismic age determination for dwarfs and giants

On the mass estimation for FGK stars: comparison of several methods

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