NY Ser: Outburst Activity and Multiperiodic Processes in its Various Stages During 2014 and 2016

Sklyanov, A. S.; Павленко, Е. П.; Antonyuk, Oksana I.; Sosnovskij, Aleksei A.; Malanushenko, Viktor; Pit, N.; Antonyuk, K. A.; Khairutdinova, A. N.; Babina, Yu. V.; Galeev, A.

doi:10.1007/s10511-018-9516-y

Cited by 9 publications

(6 citation statements)

References 24 publications

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“…It lasted about 18-19 days, including rebrightening and taking into account that the start of the superoutburst was around JD 2457216 according to the VSNET announcement. Note that this duration was the same as those of another dwarf novae in the period gap NY Ser (Pavlenko et al 2014, Sklyanov et al 2018) and MN Dra (Sklyanov et al in preparation). The amplitude of normal outbursts was a few tenths of magnitude less and varied, which is caused by the large variations of the quiescent brightness.…”

Section: Long-term Light Curve Cycles and Supercyclementioning

confidence: 62%

Long-period SU UMa dwarf nova V1006 Cygni outburst activity and variability at different brightness states in 2015-2017

Pavlenko,

Shugarov,

Simon

et al. 2018

Preprint

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CCD photometric observations of the dwarf nova V1006 Cyg were carried out in 2015 -2017 with 11 telescopes located at 7 observatories. They covered the 2015 superoutburst with rebrightening, five normal outbursts of ∼ 4-day duration and one wide outburst that lasted at least seven days. The interval between normal outbursts was 16 and 22 days, and between superoutbursts is expected to be longer than 124 days. The positive superhumps with the mean period of 0 d .10544(10) and 0 d .10406(17) were detected during the 2015 superoutburst and during the short-term quiescence between rebrightening and the start of the first normal outburst, respectively. During a wide 2017 outburst the orbital period 0 d .09832(15) was found. The amplitude of this signal was ∼ 2.5 times larger at the outburst decline than at its end. During the quiescence stage between the first and the second normal outbursts in 2015 we possibly detected the negative superhumps with the period of 0 d .09714(7).

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Section: Long-term Light Curve Cycles and Supercyclementioning

confidence: 62%

Long-period SU UMa dwarf nova V1006 Cygni outburst activity and variability at different brightness states in 2015-2017

Pavlenko,

Shugarov,

Simon

et al. 2018

Preprint

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“…The refined relation was shown in Kato et al (2016b) and Kato et al (2017a) [we consider that Kato et al (2017a) to be the final regular summary of the statistics]. The stage A, B and C are now well-established and used in many publications by various authors: Katysheva et al (2014Katysheva et al ( ), B ąkowska et al (2014, Sklyanov et al (2016), Neustroev et al (2017), Ba ¸kowska et al (2017), Neustroev et al (2018), Sklyanov et al (2018), Littlefield et al (2018), Pala et al (2018), Pala et al (2019), Pavlenko et al (2019), McAllister et al (2019), Court et al (2019) (this work also illustrates the difficulty in determining superhump times in a deeply eclipsing system). The rapid growth of papers referring to our superhump stages indicates that this concept and application are now widely accepted in this field.…”

Section: Su Uma-type Dwarf Novae and Superhump Stagesmentioning

confidence: 95%

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. X: The Tenth Year (2017)

Kato,

Isogai,

Wakamatsu

et al. 2019

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Continuing the project described by Kato et al. (2009, PASJ, 61, S395), we collected times of superhump maxima for 102 SU UMa-type dwarf novae observed mainly during the 2017 season and characterized these objects. WZ Sge-type stars identified in this study are PT And, ASASSN-17ei, ASASSN-17el, ASASSN-17es, ASASSN-17fn, ASASSN-17fz, ASASSN-17hw, ASASSN-17kd, ASASSN-17la, PNV J20205397+2508145 and TCP J00332502−3518565. We obtained new mass ratios for 7 objects using growing superhumps (stage A). ASASSN-17gf is an EI Psc-type object below the period minimum. CRTS J080941.3+171528 and DDE are objects in the period gap and both showed long-lasting phase of stage A superhumps. We also summarized the recent advances in understanding of SU UMa-type and WZ Sge-type dwarf novae.

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“…NY Ser is an object in the period gap (Nogami et al 1998;Sklyanov et al 2018). It has been shown that "longnormal" outbursts (long outbursts without superhumps) were recorded in this object (Pavlenko et al 2014).…”

Section: Behavior Near Limit Of Tidal Stabilitymentioning

confidence: 99%

“…It may be, however, worth noting that long superhump period of 0.10516(3) d was detected during the post-superoutburst phase (with dwarf nova outbursts) between BJD 2458213 and 2458222 (see E-figure 3 in SI). The fractional superhump excess (in frequency) ǫ * ≡ 1 − P orb /P SH , where P SH is the superhump period, was very large [0.0723(2)] using P orb =0.097558(6) d in Sklyanov et al (2018). If this long superhump period reflects the dynamical precession rate (i.e.…”

Section: Superhumpsmentioning

confidence: 99%

Discovery of Standstills in the SU UMa-Type Dwarf Nova NY Serpentis

Kato,

Pavlenko,

Pit

et al. 2019

Preprint

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We found that the SU UMa-type dwarf nova NY Ser in the period gap [orbital period 0.097558(6) d] showed standstills twice in 2018. This is the first clear demonstration of a standstill occurring between superoutbursts of an SU UMa-type dwarf nova. There was no sign of superhumps during the standstill, and at least one superoutburst directly started from the standstill. This provides strong evidence that the 3:1 resonance was excited during standstills. This phenomenon indicates that the disk radius can grow during standstills. We also interpret that the condition close to the limit of the tidal instability caused early quenching of superoutbursts, which resulted substantial amount of matter left in the disk after the superoutburst. We interpret that the substantial matter in the disk in condition close to the limit of the tidal instability is responsible for standstills (as in the high mass-transfer system NY Ser) or multiple rebrightenings (as in the low mass-transfer system V1006 Cyg).

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NY Ser: Outburst Activity and Multiperiodic Processes in its Various Stages During 2014 and 2016

Cited by 9 publications

References 24 publications

Long-period SU UMa dwarf nova V1006 Cygni outburst activity and variability at different brightness states in 2015-2017

Long-period SU UMa dwarf nova V1006 Cygni outburst activity and variability at different brightness states in 2015-2017

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. X: The Tenth Year (2017)

Discovery of Standstills in the SU UMa-Type Dwarf Nova NY Serpentis

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