1RXS J232953.9+062814 was identified as a cataclysmic variable by Wei et al .
( 1999 ) .
Four low-resolution spectra of 1RXS J232953.9+062814 were obtained by using the 2.16-m telescope of the National Astronomical Observatories , in which two of them were at outburst , and the other two were at quiescence .
The system is about 16.8 B and 16.5 V at quiescence , and 12.6 B and 12.6 V at outburst .
The quiescent spectra were dominated by double-peaked Balmer emissions , which indicates a hydrogen-rich system with a high-inclination accretion disc .
MgH and TiO absorption bands appeared in the quiescent spectrum imply a companion with a spectral type of early M dwarf .
If we take it as a M0 dwarf , the system is located at a distance of 350 pc with a proper motion velocity 150 km s ^ { -1 } .
The superhump period of 0.046311 days ( Uemura et al .
2001 ) was confirmed by our V photometry .
The short period and the hydrogen-rich nature reveal that this system is another SU Ursae Majoris-type dwarf nova below the period minimum after V485 Centauri .
1RXS J232953.9+062814 is one of the most important systems for studying the evolutionary scenario of cataclysmic variables since it is much brighter than V485 Cen .