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Establishing the accuracy of asteroseismic mass and radius estimates of giant stars – I. Three eclipsing systems at [Fe/H] ∼ −0.3 and the need for a large high-precision sample

Brogaard, K. and Hansen, C. J. and Miglio, A. and Slumstrup, D. and Frandsen, S. and Jessen-Hansen, J. and Lund, M. N. and Bossini, D. and Thygesen, A. and Davies, G. R. and Chaplin, W. J. and Arentoft, T. and Bruntt, H. and Grundahl, F. and Handberg, R. (2018) Establishing the accuracy of asteroseismic mass and radius estimates of giant stars – I. Three eclipsing systems at [Fe/H] ∼ −0.3 and the need for a large high-precision sample. Monthly Notices of the Royal Astronomical Society, 476 (3). pp. 3729-3743. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20180516-150008058

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Abstract

We aim to establish and improve the accuracy level of asteroseismic estimates of mass, radius, and age of giant stars. This can be achieved by measuring independent, accurate, and precise masses, radii, effective temperatures and metallicities of long period eclipsing binary stars with a red giant component that displays solar-like oscillations. We measured precise properties of the three eclipsing binary systems KIC 7037405, KIC 9540226, and KIC 9970396 and estimated their ages be 5.3 ± 0.5, 3.1 ± 0.6, and 4.8 ± 0.5 Gyr. The measurements of the giant stars were compared to corresponding measurements of mass, radius, and age using asteroseismic scaling relations and grid modelling. We found that asteroseismic scaling relations without corrections to Δν systematically overestimate the masses of the three red giants by 11.7 per cent, 13.7 per cent, and 18.9 per cent, respectively. However, by applying theoretical correction factors fΔν according to Rodrigues et al. (2017), we reached general agreement between dynamical and asteroseismic mass estimates, and no indications of systematic differences at the precision level of the asteroseismic measurements. The larger sample investigated by Gaulme et al. (2016) showed a much more complicated situation, where some stars show agreement between the dynamical and corrected asteroseismic measures while others suggest significant overestimates of the asteroseismic measures. We found no simple explanation for this, but indications of several potential problems, some theoretical, others observational. Therefore, an extension of the present precision study to a larger sample of eclipsing systems is crucial for establishing and improving the accuracy of asteroseismology of giant stars.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty268DOIArticle
ORCID:
AuthorORCID
Brogaard, K.0000-0003-2001-0276
Slumstrup, D.0000-0003-4538-9518
Thygesen, A.0000-0002-4912-1183
Chaplin, W. J.0000-0002-5714-8618
Additional Information:© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2018 January 23. Received 2018 January 23; in original form 2017 August 25. Published: 01 February 2018. We thank the anonymous referee for useful comments that helped improve the paper. Based in part on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). The research was supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no. 267864). AM, GRD, KB and WJC acknowledge the support of the UK Science and Technology Facilities Council (STFC). This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.
Funders:
Funding AgencyGrant Number
Danish National Research FoundationDNRF106
European Research Council (ERC)267864 ASTERISK
Science and Technology Facilities Council (STFC)UNSPECIFIED
NASANAS5-26555
NASANNX09AF08G
Subject Keywords:binaries: eclipsing – stars: evolution – stars: fundamental parameters – stars: individual: KIC 7037405, KIC 9540226, KIC 9970396 – Galaxy: stellar content
Record Number:CaltechAUTHORS:20180516-150008058
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20180516-150008058
Official Citation:K Brogaard, C J Hansen, A Miglio, D Slumstrup, S Frandsen, J Jessen-Hansen, M N Lund, D Bossini, A Thygesen, G R Davies, W J Chaplin, T Arentoft, H Bruntt, F Grundahl, R Handberg; Establishing the accuracy of asteroseismic mass and radius estimates of giant stars – I. Three eclipsing systems at [Fe/H] ∼ −0.3 and the need for a large high-precision sample, Monthly Notices of the Royal Astronomical Society, Volume 476, Issue 3, 21 May 2018, Pages 3729–3743, https://doi.org/10.1093/mnras/sty268
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:86429
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:18 May 2018 17:19
Last Modified:18 May 2018 17:19

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