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

Abstract

KOI-3890 is a highly eccentric, 153-day 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 have enabled the detailed characterisation 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 $M_{\star }=1.04\pm 0.06{\text{M}}_{\odot }$ and $R_{\star }=5.8\pm 0.2{\text{R}}_{\odot }$ respectively. When combined with transit photometry the M-dwarf companion is found to have a mass and radius of $M_{\mathrm{c}}=0.23\pm 0.01{\text{M}}_{\odot }$ and $R_{\mathrm{c}}=0.256\pm 0.007{\text{R}}_{\odot }$. Moreover, through asteroseismology we constrain the age of the system through the red-giant primary to be $9.1_{-1.7}^{+2.4}\mathrm{Gyr}$. 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 $i=87.6_{-1.2}^{+2.4}$ degrees. The obliquity of the system\textemdash the angle between the stellar rotation axis and the angle normal to the orbital plane\textemdash is also derived to give $\psi =4.2_{-4.2}^{+2.1}$ 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.

11 pages, 5 figures, accepted for publication in MNRAS

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