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

Abstract

We identify HS 2325+8205 as an eclipsing, frequently outbursting dwarf nova with an orbital period of 279.841731(5) min. Spectroscopic observations are used to derive the radial velocity curve of the secondary star from absorption features and also from the H-alpha emission lines, originating from the accretion 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 outburst recurrence time of 12-14 d, The combination of magnitude range (17-14 mag), high declination, eclipsing nature and frequency of outbursts makes HS 2325+8205 the ideal system for "real-time" studies of the accretion disc evolution and behavior in dwarf nova outbursts.

20 pages, 7 figures. Accepted for Publications of the Astronomical Society of the Pacific

References in corpus (4)

• The Evolution of Cataclysmic Variables as Revealed by their Donor Stars
• A brown dwarf mass donor in an accreting binary
• HS2237+8154: On the onset of mass transfer or entering the period gap?
• ULTRACAM observations of SDSS J170213.26+322954.1 - an eclipsing cataclysmic variable in the period gap

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• First discovery of QPOs in the dwarf nova HS 2325+8205 based on TESS photometry
• Nine New Cataclysmic Variable Stars with Negative Superhumps
• The Z Camelopardalis-type star AY Piscium: stellar and accretion disk parameters
• Tilted Disk Precession and Negative Superhumps in HS 2325+8205: A Multi-Window Analysis