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We observed a new and poorly studied cataclysmic variable (CV) SDSSJ123813.73-033933.0 to determine its classification and binary parameters.Simultaneous time-resolved photometric and spectroscopic observations werecarried out to conduct period analysis and Doppler tomography mapping. Fromradial velocity measurements of the Ha line we determined its orbital period tobe 0.05592+/-0.00035$ days (80.53min). This period is longer than the firstestimate of 76 min by Szkody et al. (2003), but still at the very edge of theperiod limit for hydrogen-rich CVs. The spectrum shows double-peaked Balmeremission lines flanked by strong broad Balmer absorption, indicating a dominantcontribution by the white dwarf primary star, and is similar to the spectra ofshort-period low-mass transfer WZ Sge-like systems. The photometric light curveshows complex variability. The system undergoes cyclic brightening up to 0.4mags, which are of semi-periodic nature with periods of the order of 8-12hours. We also detect a 40.25 min variability of ~0.15 mag corresponding tohalf of the orbital period. Amplitude of the latter increases with the cyclicbrightening of the system. We discuss the variable accretion rate and itsimpact 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 shortperiod system with low and unstable accretion rate.Comment: 9 pages, 7 figures, accepted to A&

Time-resolved observations of the short period CV SDSS J123813.73-033933.0