  We present observations and analysis of a new eclipsing binary HBHA 4705-03.
Using decomposition of the light curve into accretion disk and hot spot
components, we estimated photometrically the mass ratio of the studied system
to be q=0.62 +-0.07. Other fundamental parameters was found with modeling. This
approach gave: white dwarf mass M_1 = (0.8 +- 0.2) M_sun, secondary mass
M_2=(0.497 +- 0.05) M_sun, orbital radius a=1.418 R_sun, orbital inclination i
= (81.58 +- 0.5) deg, accretion disk radius r_d/a = 0.366 +- 0.002, and
accretion rate dot{M} = (2.5 +- 2) * 10^{18}[g/s], (3*10^{-8} [M_sun/yr]).
Power spectrum analysis revealed ambiguous low-period Quasi Periodic
Oscillations centered at the frequencies f_{1}=0.00076 Hz, f_2=0.00048 Hz and
f_3=0.00036 Hz. The B-V=0.04 [mag] color corresponds to a dwarf novae during an
outburst. The examined light curves suggest that HBHA 4705-03 is a nova-like
variable star.
