  We observed a new and poorly studied cataclysmic variable (CV) SDSS
J123813.73-033933.0 to determine its classification and binary parameters.
Simultaneous time-resolved photometric and spectroscopic observations were
carried out to conduct period analysis and Doppler tomography mapping. From
radial velocity measurements of the Ha line we determined its orbital period to
be 0.05592+/-0.00035$ days (80.53min). This period is longer than the first
estimate of 76 min by Szkody et al. (2003), but still at the very edge of the
period limit for hydrogen-rich CVs. The spectrum shows double-peaked Balmer
emission lines flanked by strong broad Balmer absorption, indicating a dominant
contribution by the white dwarf primary star, and is similar to the spectra of
short-period low-mass transfer WZ Sge-like systems. The photometric light curve
shows complex variability. The system undergoes cyclic brightening up to 0.4
mags, which are of semi-periodic nature with periods of the order of 8-12
hours. We also detect a 40.25 min variability of ~0.15 mag corresponding to
half of the orbital period. Amplitude of the latter increases with the cyclic
brightening of the system. We discuss the variable accretion rate and its
impact on the hot spot as the most probable reason for both observed processes.
SDSS J123813.73-033933.0 is preliminary classified as a WZ Sge-like short
period system with low and unstable accretion rate.
