  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. 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 Teff 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. NSVS 10653195 is a detached
eclipsing binary composed of two similar stars with masses of
M1=0.6402+/-0.0052 Msun and M2=0.6511+/-0.0052 Msun and radii of
R1=0.687^{+0.017}_{-0.024} Rsun and R2=0.672^{+0.018}_{-0.022} Rsun. Spectral
types were estimated to be K6V and K7V. These stars rotate in a circular orbit
with an orbital inclination of i=86.22+/-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)~8 based on the Mbol-log Teff diagram. NSVS 10653195 is composed of two
oversized and active K stars. While their radii is above model predictions
their Teff are in better agreement with models.
