IX Draconis - a curious ER UMa-type dwarf nova

• Published in: Monthly notices of the Royal Astronomical Society 2013-02, Vol.429 (1), p.868-880
• Main Authors: Otulakowska-Hypka, M., Olech, A., de Miguel, E., Rutkowski, A., Koff, R., B kowska, K.
• Format: Article
• Language: English
• Subjects: Astrophysics; Dwarf stars; Spectrum analysis; Star & galaxy formation; Statistics
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/sts385

We report results of an extensive worldwide observing campaign devoted to a very active dwarf nova star - IX Draconis. We investigated photometric behaviour of the system to derive its basic outburst properties and understand peculiarities of IX Draconis as well as other active cataclysmic variables, in particular dwarf novae of the ER UMa type. In order to measure fundamental parameters of the system, we carried out analyses of the light curve, O − C diagram, and power spectra. During over two months of observations, we detected two superoutbursts and several normal outbursts. The V magnitude of the star varied in the range 14.6-18.2 mag. Superoutbursts occur regularly with the supercycle length (P sc) of 58.5 ± 0.5 d. When analysing data over the past 20 years, we found that P sc is increasing at a rate of . Normal outbursts appear to be irregular, with typical occurrence times in the range 3.1-4.1 d. We detected a double-peaked structure of superhumps during superoutburst, with the secondary maximum becoming dominant near the end of the superoutburst. The mean superhump period observed during superoutbursts is P sh = 0.066982(36) d (96.45 ± 0.05 min), which is constant over the last two decades of observations. Based on the power spectrum analysis, the evaluation of the orbital period was problematic. We found two possible values: the first one, 0.066 41(3) d (95.63 ± 0.04 min), which is in agreement with previous studies and our O − C analysis [0.06646(2) d, 95.70 ± 0.03 min], and the second one, 0.06482(3) d (93.34 ± 0.04 min), which is less likely. The evolutionary status of the object depends dramatically on the choice between these two values. A spectroscopic determination of the orbital period is needed. We updated available information on ER UMa-type stars and present a new set of their basic statistics. Thereby, we provide evidence that this class of stars is not uniform.