Abstract
ABSTRACTWe identify HS 2325 + 8205 as an eclipsing, frequently outbursting, dwarf nova with an orbital period of Porb = 279.841731(5) minutes. Spectroscopic observations are used to derive the radial velocity curve of the secondary star from absorption features and also from the Hα emission lines, originating from the accretion disk, yielding Ksec = Kabs = 237 ± 28 km s-1 and Kem = 145 ± 9 km s-1, respectively. The distance to the system is calculated to be 400(+200,-140) pc. A photometric monitoring campaign reveals an outburst recurrence time of ∼12–14 days. The combination of magnitude range (17–14 mag), high declination, and eclipsing nature and frequency of outbursts makes HS 2325 + 8205 the ideal system for “real-time” studies of the accretion disk evolution and behavior in dwarf nova outbursts.
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