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Asteroseismic scaling relations can provide high-precision measurements ofmass and radius for red giant (RG) stars displaying solar-like oscillations.Their accuracy can be validated and potentially improved using independent andaccurate observations of mass, radius, effective temperature and metallicity.We seek to achieve this using long period SB2 eclipsing binaries hostingoscillating RGs. We explore KIC 8430105, for which a previous study foundsignificant asteroseismic overestimation of mass and radius when compared witheclipsing binary measurements. We measured dynamical masses and radii for bothcomponents to be significantly lower than previously established, increasingthe discrepancy between asteroseismic and dynamical measurements. Our dynamicalmeasurements of the RG component were compared to corresponding measurements ofmass and radius using asteroseismic scaling relations. Uncorrected scalingrelations overestimated the mass of the RG by 26%, the radius by 11%, and theaverage density by 7%, in agreement with studies for other systems. However,using a theoretical correction to $\Delta \nu$, we managed to obtain anasteroseismic average density that is $1\sigma$ consistent with our dynamicalresult. We obtained several measurements of $\nu_{max}$ that are not fullyconsistent. With $\nu_{max} = 76.78 \pm 0.81\mu $Hz, the $\Delta \nu$correction provided $2 \sigma$ consistent mass and radius for the giant. Theage of the system was estimated to be $3.7 \pm 0.4$ Gyr.

Establishing the accuracy of asteroseismic mass and radius estimates of giant stars. II. Revised stellar masses and radii for KIC 8430105