Context : Low-mass stars in eclipsing binary systems show radii larger and effective temperatures lower than theoretical stellar models predict for isolated stars with the same masses .
Eclipsing binaries with low-mass components are hard to find due to their low luminosity .
As a consequence , the analysis of the known low-mass eclipsing systems is key to understand this behavior .

Aims : We aim to investigate the mass–radius relation for low-mass stars and the cause of the deviation of the observed radii in low-mass detached eclipsing binary stars ( LMDEB ) from theoretical stellar models .

Methods : We developed a physical model of the LMDEB system NSVS 10653195 to accurately measure the masses and radii of the components .
We obtained several high-resolution spectra in order to fit a spectroscopic orbit .
Standardized absolute photometry was obtained to measure reliable color indices and to measure the mean T _ { eff } of the system in out-of-eclipse phases .
We observed and analyzed optical VRI and infrared JK band differential light-curves which were fitted using PHOEBE .
A Markov-Chain Monte Carlo ( MCMC ) simulation near the solution found provides robust uncertainties for the fitted parameters .

Results : NSVS 10653195 is a detached eclipsing binary composed of two similar stars with masses of M _ { 1 } = 0.6402 \pm 0.0052 M _ { \sun } and M _ { 2 } = 0.6511 \pm 0.0052 M _ { \sun } and radii of R _ { 1 } = 0.687 ^ { +0.017 } _ { -0.024 } R _ { \sun } and R _ { 2 } = 0.672 ^ { +0.018 } _ { -0.022 } R _ { \sun } .
Spectral types were estimated to be K6V and K7V .
These stars rotate in a circular orbit with an orbital inclination of i = 86.22 \pm 0.61 degrees and a period of P = 0.5607222 ( 2 ) d. The distance to the system is estimated to be d = 135.2 ^ { +7.6 } _ { -7.9 } pc , in excellent agreement with the value from Gaia .
If solar metallicity were assumed , the age of the system would be older than \log ( age ) \sim 8 based on the M _ { bol } - \log T _ { eff } diagram .

Conclusions : NSVS 10653195 is composed of two oversized and active K stars .
While their radii is above model predictions their T _ { eff } are in better agreement with models .