Repozytorium Uniwersytetu Jagiellońskiego

IX Draconis – a curious ER UMa-type dwarf nova

IX Draconis – a curious ER UMa-type dwarf nova

Metadane (Dublin Core)

dc.contributor.author Otulakowska-Hypka, M. pl
dc.contributor.author Olech, A. pl
dc.contributor.author Miguel, E. de pl
dc.contributor.author Rutkowski, Artur [SAP14010185] pl
dc.contributor.author Koff, R. pl
dc.contributor.author Bąkowska, K. pl
dc.date.accessioned 2015-06-29T14:03:30Z
dc.date.available 2015-06-29T14:03:30Z
dc.date.issued 2013 pl
dc.identifier.issn 0035-8711 pl
dc.identifier.uri http://ruj.uj.edu.pl/xmlui/handle/item/10657
dc.language eng pl
dc.title IX Draconis – a curious ER UMa-type dwarf nova pl
dc.type JournalArticle pl
dc.description.physical 868-880 pl
dc.abstract.en 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 \pm 0.5 d. When analysing data over the past 20 years, we found that (P_{sc}) is increasing at a rate of \dot{P}=1.8 \times 10^{-3}. 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 \pm 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 \pm 0.04 min), which is in agreement with previous studies and our O − C analysis [0.06646(2) d, 95.70 \pm 0.03 min], and the second one, 0.06482(3) d (93.34 \pm 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. pl
dc.subject.en binaries: close pl
dc.subject.en stars: dwarf novae pl
dc.subject.en stars: individual: IX Draconis pl
dc.description.volume 429 pl
dc.description.number 1 pl
dc.identifier.doi 10.1093/mnras/sts385 pl
dc.identifier.eissn 1365-2966 pl
dc.title.journal Monthly Notices of the Royal Astronomical Society pl
dc.language.container eng pl
dc.affiliation Wydział Fizyki, Astronomii i Informatyki Stosowanej : Instytut – Obserwatorium Astronomiczne pl
dc.subtype Article pl
dc.rights.original OTHER; inne; ostateczna wersja wydawcy; po opublikowaniu; 36; pl
.pointsMNiSW [2013 A]: 35


Pliki tej pozycji

Plik Rozmiar Format Przeglądanie

Nie ma plików powiązanych z tą pozycją.

Pozycja umieszczona jest w następujących kolekcjach