Curious Variables Experiment (CURVE) CCD photometry of QW Serpentis in superoutburst and quiescence

Olech, A.; Kêdzierski, P.; Złoczewski, K.; Mularczyk, K.; Wiśniewski, M.

doi:10.1051/0004-6361:20034080

Cited by 44 publications

(109 citation statements)

References 9 publications

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“…One of the most important findings is the fact that the supercycle length of IX Dra continually increases during the past twenty years and is now equal to 58.5 ± 0.5 d. See Data points are taken from Klose 1995, Ishioka et al 2001, and Olech et al 2004 We detected double humps during superoutburst, with the secondary maximum peaking near the end of the superoutburst. They appeared with the same superhump period, which is constant for IX Dra over the last twenty years and is equal to P sh = 0.066982 (36) (2)).…”

Section: Overviewmentioning

confidence: 79%

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IX Draconis, ER UMa-type dwarf nova

Otulakowska-Hypka¹,

Olech²,

Miguel

et al. 2012

Proc. IAU

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Abstract. We present results of our world-wide observing campaign which was dedicated to one of the most active dwarf novae, IX Draconis. We investigated photometric behaviour of the system to derive its basic parameters. This study is important in the context of our understanding of the accretion process of IX Draconis, as well as other active cataclysmic variables, especially those from the still poorly studied type of ER UMa stars.

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Section: Overviewmentioning

confidence: 79%

“…Up to now we know only five stars belonging to the ER UMa-type of stars: ER UMa (Kato et al 1995), V1159 Ori (Patterson et al 1995, Szkody et al 1999, RZ LMi (Olech et al 2008), DI UMa (Rutkowski et al 2009), and IX Dra (Olech et al 2004). Therefore, studying each of them is extremely important.…”

Section: Introductionmentioning

confidence: 99%

IX Draconis, ER UMa-type dwarf nova

Otulakowska-Hypka¹,

Olech²,

Miguel

et al. 2012

Proc. IAU

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“…Kato et al (2003b) noticed an exceptionally large period decrease of superhumps, and was considered to be a prototypical SU UMa-type dwarf nova with a large period decrease and this result was often referred for comparison [cf. MN Dra (Nogami et al 2003); KS UMa (Olech et al 2003); V419 Lyr (Rutkowski et al 2007)]. This detection of a large period decrease was before the establishment of the common pattern of period variations (stages A-C, Kato et al 2009), and it has been clarified that the large period decrease in KK Tel was likely a result of stage A-B transition.…”

Section: Kk Telescopiimentioning

confidence: 98%

Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015–2016)

Katô

Hambsch

Monard

et al. 2016

Publications of the Astronomical Society of Japan

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Continuing the project described by Kato et al. (2009), we collected times of superhump maxima for 128 SU UMa-type dwarf novae observed mainly during the 2015-2016 season and characterized these objects. The data have improved the distribution of orbital periods, the relation between the orbital period and the variation of superhumps, the relation between period variations and the rebrightening type in WZ Sge-type objects. Coupled with new measurements of mass ratios using growing stages of superhumps, we now have a clearer and statistically greatly improved evolutionary path near the terminal stage of evolution of cataclysmic variables. Three objects (V452 Cas, KK Tel, ASASSN-15cl) appear to have slowly growing superhumps, which is proposed to reflect the slow growth of the 3:1 resonance near the stability border. ASASSN-15sl, ASASSN-15ux, SDSS J074859.55+312512.6 and CRTS J200331.3−284941 are newly identified eclipsing SU UMa-type (or WZ Sge-type) dwarf novae. ASASSN-15cy has a short (∼0.050 d) superhump period and appears to belong to EI Psc-type objects with compact secondaries having an evolved core. ASASSN-15gn, ASASSN-15hn, ASASSN-15kh and ASASSN-16bu are candidate period bouncers with superhump periods longer than 0.06 d. We have newly obtained superhump periods for 79 objects and 13 orbital periods, including periods from early superhumps. In order that the future observations will be more astrophysically beneficial and rewarding to observers, we propose guidelines how to organize observations of various superoutbursts.

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“…These are systems characterized by an extremely short supercycle (20−60 days), a short interval between normal outbursts (3−4 days), and small amplitude (∼3 mag) of superoutbursts (Kato & Kunjaya 1995;Robertson et al 1995;Patterson et al 1995). Subsequently, one more object with similar characteristics was discovered (IX Dra - Ishioka et al 2001;Olech et al 2004a). …”

Section: Er Uma Starsmentioning

confidence: 99%

“…It is clear that only the 1999−2000 behavior fits the Kukarkin-Parenago relation well. Another empirical relation followed by dwarf novae connects their cycle and supercycle lenghts (Patterson et al 1995;Warner 1995;Olech et al 2004a):…”

Section: Another Possibility For Ss Umi?mentioning

confidence: 99%

The CUrious Variables Experiment (CURVE). Variable properties of the dwarf nova SS Ursae Minoris

Olech¹,

Mularczyk

Kêdzierski

et al. 2006

A&A

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We report on extensive photometry of the dwarf nova SS Ursae Minoris throughout nine months of 2004. In total, we recorded two superoutbursts and 11 normal outbursts of the star. SS UMi has been known to show frequent superoutbursts with a mean interval of 84.7 days. Our data suggest that the interval between successive superoutbursts lengthened to 197 days, indicating that SS UMi entered a period of untypical behavior manifested by a growth in the quiescent magnitude of the star and a series of frequent, low-amplitude, normal outbursts observed from July to September 2004. The mean superhump period derived for the April 2004 superoutburst of SS UMi is P sh = 0.070149(16) days (101.015 ± 0.023 min). Combining this value with an earlier orbital period determination, we were able to derive the period excess, which is equal to 3.5 ± 1.6%, and estimate the mass ratio of the binary system as equal to q = 0.16 ± 0.07. During the entire superoutburst, the period decreased at a rate ofṖ/P sh = −6.3(1.4) × 10 −5 . However, detailed analysis of the timings of superhump maxima seem to suggest a more complex period change, with a decrease in the period during the first and last stages of the superoutburst but an increase in the middle interval.

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Curious Variables Experiment (CURVE) CCD photometry of QW Serpentis in superoutburst and quiescence

Cited by 44 publications

References 9 publications

IX Draconis, ER UMa-type dwarf nova

IX Draconis, ER UMa-type dwarf nova

Survey of period variations of superhumps in SU UMa-type dwarf novae. VIII. The eighth year (2015–2016)

The CUrious Variables Experiment (CURVE). Variable properties of the dwarf nova SS Ursae Minoris

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