  A 2014 study of the eclipsing binary star 1SWASPJ011351.29+314909.7
(J0113+31) reported an unexpectedly high effective temperature for the M-dwarf
companion to the 0.95-M$_{\odot}$ primary star. The effective temperature
inferred from the secondary eclipse depth was $\sim$600 K higher than the value
predicted from stellar models. Such an anomalous result questions our
understanding of low-mass stars and might indicate a significant uncertainty
when inferring properties of exoplanets orbiting them. We seek to measure the
effective temperature of the M-dwarf companion using the light curve of
J0113+31 recently observed by the Transiting Exoplanet Survey Satellite (TESS).
We use the pycheops modelling software to fit a combined transit and eclipse
model to the TESS light curve. To calculate the secondary effective
temperature, we compare the best-fit eclipse depth to the predicted eclipse
depths from theoretical stellar models. We determined the effective temperature
of the M dwarf to be ${\rm T}_{\rm eff,2}$ = 3208 $\pm$ 43 K, assuming $\log
g_2$ = 5, [Fe/H] = $-0.4$ and no alpha-element enhancement. Varying these
assumptions changes ${\rm T}_{\rm eff,2}$ by less than 100 K. These results do
not support a large anomaly between observed and theoretical low-mass star
temperatures.
