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In the hunt for Earth-like exoplanets it is crucial to have reliable hoststar parameters, as they have a direct impact on the accuracy and precision ofthe inferred parameters for any discovered exoplanet. For stars with massesbetween 0.35 and 0.5 ${\rm M_{\odot}}$ an unexplained radius inflation isobserved relative to typical stellar models. However, for fully convectiveobjects with a mass below 0.35 ${\rm M_{\odot}}$ it is not known whether thisradius inflation is present as there are fewer objects with accuratemeasurements in this regime. Low-mass eclipsing binaries present a uniqueopportunity to determine empirical masses and radii for these low-mass stars.Here we report on such a star, EBLM J2114-39\,B. We have used HARPS and FEROSradial-velocities and TESS photometry to perform a joint fit of the data, andproduce one of the most precise estimates of a very low mass star's parameters.Using a precise and accurate radius for the primary star using Gaia DR3 data,we determine J2114-39 to be a $M_1 = 0.987 \pm 0.059$ ${\rm M_{\odot}}$ primarystar hosting a fully convective secondary with mass $M_2~=~0.0986~\pm0.0038~\,\mathrm{M_{\odot}}$, which lies in a poorly populated region ofparameter space. With a radius $R_2 =~0.1275~\pm0.0020~\,\mathrm{R_{\odot}}$,similar to TRAPPIST-1, we see no significant evidence of radius inflation inthis system when compared to stellar evolution models. We speculate thatstellar models in the regime where radius inflation is observed might beaffected by how convective overshooting is treated.

The EBLM Project XII. An eccentric, long-period eclipsing binary with a companion near the hydrogen-burning limit