  HD 213597 is an eclipsing binary system which was detected by the STEREO
spacecraft and was speculated to host a low-mass stellar companion. We used
high-resolution spectroscopy with the 10-m Hobby-Eberly Telescope and the 1.2-m
telescope in Mt Abu for radial velocity (RV) measurements of this source. We
performed aperture photometry for this star on the STEREO archival data and
thereby confirm the transit signature. We also did follow-up ground-based
photometry with a 10-inch telescope from Mt Abu. The spectroscopic RV
semi-amplitude of the primary (33.39 km s^-1) indicates that the secondary is
an M dwarf making the system a short period F+M eclipsing binary. These RVs
along with the inclination derived from our combined photometric analysis
(i=84.9 degree), enable us to estimate the mass of the secondary as M_B ~ 0.286
M_sun and radius as R_B ~ 0.344 R_sun using an estimated mass M_A ~ 1.3 M_sun
and radius R_B ~ 1.97 R_sun of the primary. Our spectral analysis returned the
following parameters: T_eff = 6625 +/-121 K, [Fe/H] = -0.095 +\-0.08 and log(g)
= 3.72 +/-0.22 for the primary. When log(g) is constrained to a value of 3.96,
we derive T_eff = 6753 +/-52 K and [Fe/H] = -0.025+\-0.05.
