Photometry of the dwarf nova V503 Cyg in 2010. Orbital and other periods

Павленко, Е. П.; Samsonov, Denis; Antonyuk, Oksana I.; Андреев, М. В.; Baklanov, A. V.; Sosnovskij, Aleksei A.

doi:10.1007/s10511-012-9255-4

Cited by 14 publications

(14 citation statements)

References 15 publications

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“…The orbital period determined from the 2012 quiescent data was 0.077755(1) d. Similarly, the 2011 quiescent data (Kato et al 2013a) yielded 0.077766(5) d. A combined analysis of the 2011 and 2012 data yielded 0.0777591(2) d, which we adopted as the refined orbital period. This period is in good agreement with 0.077760(3) d reported in Pavlenko et al (2012).…”

Section: Kato Et Al 2012asupporting

confidence: 92%

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Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. V: The Fifth Year (2012-2013)

Kato,

Hambsch,

Maehara

et al. 2013

Preprint

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Continuing the project described by Kato et al. (2009a), we collected times of superhump maxima for SU UMa-type dwarf novae mainly observed during the 2012-2013 season. We found three objects (V444 Peg, CSS J203937 and MASTER J212624) having strongly positive period derivatives despite the long orbital period (P orb ). By using the period of growing stage (stage A) superhumps, we obtained mass ratios for six objects. We characterized nine new WZ Sge-type dwarf novae. We made a pilot survey of the decline rate of slowly fading part of SU UMa-type and WZ Sge-type outbursts. The decline time scale was found to generally follow the expected P 1/4 orb dependence and WZ Sge-type outbursts also generally follow this trend. There are some objects which show slower decline rates, and we consider these objects good candidates for period bouncers. We also studied unusual behavior in some objects, including BK Lyn which made a transition from an ER UMa-type state to the novalike (standstill) state in 2013 and unusually frequent occurrence of superoutbursts in NY Ser and CR Boo. We applied least absolute shrinkage and selection operator (Lasso) power spectral analysis, which has been proven to be very effective in analyzing the Kepler data, to ground-based photometry of BK Lyn and detected the dramatic disappearance of the signal of negative superhumps in 2013. We suggested that the mass-transfer rates did not vary strongly between the ER UMa-type state and novalike state in BK Lyn, and this transition was less likely caused by a systematic variation of the mass-transfer rate.

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Section: Kato Et Al 2012asupporting

confidence: 92%

“…proposed that the disk tilt, which is supposed to cause negative superhumps, is responsible for the suppression of normal outbursts. In recent years, V503 Cyg did not show distinct negative superhumps (Kato et al 2013a;Pavlenko et al 2012).…”

Section: V503 Cygnimentioning

confidence: 97%

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. V: The Fifth Year (2012-2013)

Kato,

Hambsch,

Maehara

et al. 2013

Preprint

View full text Add to dashboard Cite

show abstract

“…The orbital period derived from the 2012 quiescent data was 0.077755(1) d. Similarly, the 2011 quiescent data ) yielded 0.077766(5) d. A combined analysis of the 2011 and 2012 data yielded 0.0777591(2) d, which we adopted as a refined orbital period. This period is in agreement with 0.077760(3) d reported in Pavlenko et al (2012). Approximate cycle counts (E) after the start of the superoutburst were used.…”

Section: V503 Cygnisupporting

confidence: 84%

“…Osaki and Kato (2013a) proposed that the disk tilt, which is supposed to cause negative superhumps, is responsible for the suppression of normal outbursts. In recent years, V503 Cyg has not shown distinct negative superhumps Pavlenko et al 2012). We observed the 2012 June superoutburst, including the quiescent segments before and after this superoutburst.…”

Section: V503 Cygnimentioning

confidence: 81%

Survey of period variations of superhumps in SU UMa-type dwarf novae. V. The fifth year (2012–2013)

Katô¹,

Hambsch²,

Maehara³

et al. 2014

Publications of the Astronomical Society of Japan

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Continuing the project described in Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for SU UMa-type dwarf novae mainly observed during the 2012-2013 season. We found three objects (V444 Peg, CSS J203937, and MASTER J212624) having strongly positive period derivatives despite the long orbital period (P orb ). By using the period of growing stage (stage A) superhumps, we obtained mass ratios for six objects. We characterized nine new WZ Sge-type dwarf novae. We made a pilot survey of the decline rate in the slowly fading parts of SU UMa-type and WZ Sge-type outbursts. The decline time scale was found to generally follow an expected P 1/4 orb dependence, and WZ Sge-type outbursts also generally follow this trend. There are some objects which show slower decline rates, and we consider these objects good candidates for period bouncers. We also studied unusual behavior in some objects, including BK Lyn which made a transition from an ER UMa-type state to a novalike (standstill) state in 2013, and unusually frequent occurrences of superoutbursts in NY Ser and CR Boo. We applied the least absolute shrinkage and selection operator (Lasso) power spectral analysis, which has been proven to be very effective in analyzing the Kepler data, to the ground-based photometry of BK Lyn, and detected a dramatic disappearance of the signal of negative superhumps in 2013. We suggested that the mass-transfer rates did not strongly vary between the ER UMa-type state and novalike state in BK Lyn, and this transition was less likely caused by a systematic variation of the mass-transfer rate.

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“…For V1504 Cyg (Osaki, Kato 2013a) and V344 Lyr (Osaki, Kato 2013b) it is established that the decrease of the frequency of normal outbursts is accompanied by the negative superhumps appearance. Vice versa, the disappearing of the negative superhumps was found for V503 Cyg [Kato et al (2013), Pavlenko et al (2012)] during the stage of a frequent normal outbursts. Since NY Ser entered the stage of frequent normal outbursts after the 2013 superoutburst, we checked whether there were negative superhumps or "impulsive" negative superhumps [Osaki, Kato (2013b)] in the data in the state of relatively infrequent normal outbursts including the wide outburst.…”

Section: Periodicity Outside Superoutburstmentioning

confidence: 95%

NY Serpentis: SU UMa-type nova in the period gap with diversity of normal outbursts

Павленко

Katô

Antonyuk

et al. 2014

Publications of the Astronomical Society of Japan

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1We present photometric study of NY Ser, an in-the-gap SU UMa-type nova, in 2002 and 2013. We determined the duration of the superoutburst and the mean superhump period to be 18 d and 0.10458 d, respectively. We detected in 2013 that NY Ser showed two distinct states separated by the superoutburst. A state of rather infrequent normal outbursts lasted at least 44 d before the superoutburst and a state of frequent outbursts started immediately after the superoutburst and lasted at least for 34 d. Unlike a typical SU UMa star with bimodal distribution of the outbursts duration, NY Ser displayed a diversity of normal outbursts. In the state of infrequent outbursts, we detected a wide ∼12 d outburst accompanied by 0.098 d orbital modulation but without superhumps ever established in NY Ser. We classified this as the "wide normal outburst". The orbital period dominated both in quiescence and during normal outbursts in this state. In the state of the most frequent normal outbursts, the 0.10465 d positive superhumps dominated and co-existed with the orbital modulation. In 2002 we detected the normal outburst of "intermediate" 5-6 d duration that was also accompanied by orbital modulations.

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Photometry of the dwarf nova V503 Cyg in 2010. Orbital and other periods

Cited by 14 publications

References 15 publications

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. V: The Fifth Year (2012-2013)

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. V: The Fifth Year (2012-2013)

Survey of period variations of superhumps in SU UMa-type dwarf novae. V. The fifth year (2012–2013)

NY Serpentis: SU UMa-type nova in the period gap with diversity of normal outbursts

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