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  KOI-3890: a high-mass-ratio asteroseismic red giant+M-dwarf eclipsing binary undergoing heartbeat tidal interactions

Kuszlewicz, J. S., North, T. S. H., Chaplin, W. J., Bieryla, A., Latham, D. W., Miglio, A., et al. (2019). KOI-3890: a high-mass-ratio asteroseismic red giant+M-dwarf eclipsing binary undergoing heartbeat tidal interactions. Monthly Notices of the Royal Astronomical Society, 487(1), 14-23. doi:10.1093/mnras/stz1185.

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 Creators:
Kuszlewicz, James S.1, Author           
North, Thomas S H, Author
Chaplin, William J, Author
Bieryla, Allyson, Author
Latham, David W, Author
Miglio, Andrea, Author
Bell, Keaton J.1, Author           
Davies, Guy R, Author
Hekker, Saskia1, Author           
Campante, Tiago L, Author
Deheuvels, Sebastien, Author
Lund, Mikkel N, Author
Affiliations:
1Max Planck Research Group in Stellar Ages and Galactic Evolution (SAGE), Max Planck Institute for Solar System Research, Max Planck Society, ou_2265636              

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Free keywords: asteroseismology, techniques: photometric, binaries: eclipsing, stars: evolution, stars: fundamental parameters
 Abstract: KOI-3890 is a highly eccentric, 153-d period eclipsing, single-lined spectroscopic binary system containing a red giant star showing solar-like oscillations alongside tidal interactions. The combination of transit photometry, radial velocity observations, and asteroseismology has enabled the detailed characterization of both the red giant primary and the M-dwarf companion, along with the tidal interaction and the geometry of the system. The stellar parameters of the red giant primary are determined through the use of asteroseismology and grid-based modelling to give a mass and radius of M_{\star }=1.04± 0.06 M_{☉} and R_{\star }=5.8± 0.2 R_{☉}, respectively. When combined with transit photometry, the M-dwarf companion is found to have a mass and radius of Mc=0.23± 0.01 M_{☉} and Rc=0.256± 0.007 R_{☉}. Moreover, through asteroseismology we constrain the age of the system through the red giant primary to be 9.1^{+2.4}_{-1.7} Gyr. This provides a constraint on the age of the M-dwarf secondary, which is difficult to do for other M-dwarf binary systems. In addition, the asteroseismic analysis yields an estimate of the inclination angle of the rotation axis of the red giant star of i=87.6^{+2.4}_{-1.2} degrees. The obliquity of the system - the angle between the stellar rotation axis and the angle normal to the orbital plane - is also derived to give ψ =4.2^{+2.1}_{-4.2} degrees, showing that the system is consistent with alignment. We observe no radius inflation in the M-dwarf companion when compared to current low-mass stellar models.

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Language(s): eng - English
 Dates: 2019
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/stz1185
 Degree: -

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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 487 (1) Sequence Number: - Start / End Page: 14 - 23 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150