Testing asteroseismic scaling relations using eclipsing binaries in star clusters and the field

The accuracy of stellar masses and radii determined from asteroseismology is not known! We examine this issue for giant stars by comparing classical measurements of detached eclipsing binary systems (dEBs) with asteroseismic measurements from the Kepler mission. For star clusters, we extrapolate mea...

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Bibliographic Details
Published in:Astronomische Nachrichten 2016-09, Vol.337 (8-9), p.793-798
Main Authors: Brogaard, K., Jessen-Hansen, J., Handberg, R., Arentoft, T., Frandsen, S., Grundahl, F., Bruntt, H., Sandquist, E. L., Miglio, A., Beck, P. G., Thygesen, A. O., Kjærgaard, K. L., Haugaard, N. A.
Format: Article
Language:English
Subjects:
asteroseismology
Astrophysics
binaries: eclipsing
Double stars
Eclipsing binary stars
Giant stars
Mass transfer
Mathematical analysis
NGC 6819
open clusters and associations: general
open clusters and associations: individual (NGC 6791
open clusters and associations: individual (NGC 6791, NGC 6819)
Red giant stars
Star clusters
stars: fundamental parameters
stars: oscillations
Stellar age
Stellar system evolution
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Summary:The accuracy of stellar masses and radii determined from asteroseismology is not known! We examine this issue for giant stars by comparing classical measurements of detached eclipsing binary systems (dEBs) with asteroseismic measurements from the Kepler mission. For star clusters, we extrapolate measurements of dEBs in the turn‐off region to the red giant branch and the red clump where we investigate the giants as an ensemble. For the field stars, we measure dEBs with an oscillating giant component. These measurements allow a comparison of masses and radii calculated from a classical eclipsing binary analysis to those calculated from asteroseismic scaling relations and/or other asteroseismic methods. Our first results indicate small but significant systematic differences between the classical and asteroseismic measurements. In this contribution we show our latest results and summarize the current status and future plans. We also stress the importance of realizing that for giant stars mass cannot always be translated to age, since an unknown fraction of these evolved through a blue straggler phase with mass transfer in a binary system. Rough estimates of how many such stars to expect are given based on our findings in the open clusters NGC 6819 and NGC 6791.
ISSN:0004-6337
1521-3994
DOI:10.1002/asna.201612374