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KOI-3890 is a highly eccentric, 153-day period eclipsing, single-linedspectroscopic binary system containing a red-giant star showing solar-likeoscillations alongside tidal interactions. The combination of transitphotometry, radial velocity observations, and asteroseismology have enabled thedetailed characterisation of both the red-giant primary and the M-dwarfcompanion, along with the tidal interaction and the geometry of the system. Thestellar parameters of the red-giant primary are determined through the use ofasteroseismology and grid-based modelling to give a mass and radius of$M_{\star}=1.04\pm0.06\;\textrm{M}_{\odot}$ and$R_{\star}=5.8\pm0.2\;\textrm{R}_{\odot}$ respectively. When combined withtransit photometry the M-dwarf companion is found to have a mass and radius of$M_{\mathrm{c}}=0.23\pm0.01\;\textrm{M}_{\odot}$ and$R_{\mathrm{c}}=0.256\pm0.007\;\textrm{R}_{\odot}$. Moreover, throughasteroseismology we constrain the age of the system through the red-giantprimary to be $9.1^{+2.4}_{-1.7}\;\mathrm{Gyr}$. This provides a constraint onthe age of the M-dwarf secondary, which is difficult to do for other M-dwarfbinary systems. In addition, the asteroseismic analysis yields an estimate ofthe 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\textemdash theangle between the stellar rotation axis and the angle normal to the orbitalplane\textemdash is also derived to give $\psi=4.2^{+2.1}_{-4.2}$ degreesshowing that the system is consistent with alignment. We observe no radiusinflation in the M-dwarf companion when compared to current low-mass stellarmodels.

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