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We identify HS 2325+8205 as an eclipsing, frequently outbursting dwarf novawith an orbital period of 279.841731(5) min. Spectroscopic observations areused to derive the radial velocity curve of the secondary star from absorptionfeatures and also from the H-alpha emission lines, originating from theaccretion disc, yielding K_secondary = K_abs = 237 +- 28 km/s and K_emn = 145+- 9 km/s respectively. The distance to the system is calculated to be 400(+200, -140) pc. A photometric monitoring campaign reveals an outburstrecurrence time of 12-14 d, The combination of magnitude range (17-14 mag),high declination, eclipsing nature and frequency of outbursts makes HS2325+8205 the ideal system for "real-time" studies of the accretion discevolution and behavior in dwarf nova outbursts.

HS 2325+8205 - an ideal laboratory for accretion disk physics