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dc.contributor.authorAviles, A.
dc.contributor.authorZharikov, S.
dc.contributor.authorTovmassian, G.
dc.contributor.authorMichel, R.
dc.contributor.authorTapia, M.
dc.contributor.authorRoth, M.
dc.contributor.authorNeustroev, V.
dc.contributor.authorZurita, C.
dc.contributor.authorAndreev, M.
dc.contributor.authorSergeev, A.
dc.contributor.authorPavlenko, E.
dc.contributor.authorTsymbal, V.
dc.contributor.authorAnupama, G. C.
dc.contributor.authorKamath, U. S.
dc.contributor.authorSahu, D. K.
dc.identifier.citationAviles, A. Zharikov, S.; Tovmassian, G.; Michel, R.; Tapia, M.; Roth, M.; Neustroev, V.; Zurita, C.; Andreev, M.; Sergeev, A.; Pavlenko, E.; Tsymbal, V.; Anupama, G. C.; Kamath, U. S.; Sahu, D. K. (2010). Sdss j123813.73 – 033933.0: a cataclysmic variable evolved beyond the period minimum. The Astrophysical Journal 711 (1), 389-398
dc.description.abstractWe present infrared JHK photometry of the cataclysmic variable (CV) SDSS J123813.73-033933.0 and analyze it along with optical spectroscopy, demonstrating that the binary system is most probably comprised of a massive white dwarf with T(eff) = 12000 +/- 1000 K and a brown dwarf of spectral type L4. The inferred system parameters suggest that this system may have evolved beyond the orbital period minimum and is a bounce-back system. SDSS J123813.73-033933.0 stands out among CVs by exhibiting the cyclical variability that Zharikov et al. called brightenings. These are not related to specific orbital phases of the binary system and are fainter than dwarf novae outbursts that usually occur on longer timescales. This phenomenon has not been observed extensively and, thus, is poorly understood. The new time-resolved, multi-longitude photometric observations of SDSS J123813.73-033933.0 allowed us to observe two consecutive brightenings and to determine their recurrence time. The period analysis of all observed brightenings during 2007 suggests a typical timescale that is close to a period of similar to 9.3 hr. However, the brightenings modulation is not strictly periodic, possibly maintaining coherence only on timescales of several weeks. The characteristic variability with double orbital frequency that clearly shows up during brightenings is also analyzed. The Doppler mapping of the system shows the permanent presence of a spiral arm pattern in the accretion disk. A simple model is presented to demonstrate that spiral arms in the velocity map appear at the location and phase corresponding to the 2: 1 resonance radius and constitute themselves as double-humped light curves. The long-term and short-term variability of this CV is discussed together with the spiral arm structure of an accretion disk in the context of observational effects taking place in bounce-back systems.
dc.publisherIOP Publishing
dc.relation.ispartofThe Astrophysical Journal
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Ireland
dc.subjectbrown dwarfs
dc.subjectnovae, cataclysmic variables
dc.subjectstars: dwarf novae
dc.subjectstars: individual
dc.subjectdwarf spectroscopic survey
dc.subjectaccretion discs
dc.subjectbrown dwarf
dc.subjectsph simulations
dc.subjectspiral shocks
dc.titleSdss j123813.73 – 033933.0: a cataclysmic variable evolved beyond the period minimum

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