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

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

doi:10.1051/0004-6361:20054483

Cited by 15 publications

(16 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…(v) Additional photometric data from our observational campaigns for eight objects (Olech et al (2003), Olech et al (2004), Olech et al (2006), Olech et al (2008, Olech et al (2009), Olech et al (2011).…”

Section: Data Sourcesmentioning

confidence: 99%

Statistical analysis of properties of dwarf novae outbursts

Otulakowska-Hypka

Olech

Patterson

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present a statistical study of all measurable photometric features of a large sample of dwarf novae during their outbursts and superoutbursts. We used all accessible photometric data for all our objects to make the study as complete and up-to-date as possible. Our aim was to check correlations between these photometric features in order to constrain theoretical models which try to explain the nature of dwarf novae outbursts. We managed to confirm a few of the known correlations, that is the Stolz and Schoembs Relation, the Bailey Relation for long outbursts above the period gap, the relations between the cycle and supercycle lengths, amplitudes of normal and superoutbursts, amplitude and duration of superoutbursts, outburst duration and orbital period, outburst duration and mass ratio for short and normal outbursts, as well as the relation between the rise and decline rates of superoutbursts. However, we question the existence of the Kukarkin-Parenago Relation but we found an analogous relation for superoutbursts. We also failed to find one presumed relation between outburst duration and mass ratio for superoutbursts. This study should help to direct theoretical work dedicated to dwarf novae.

show abstract

Section: Data Sourcesmentioning

confidence: 99%

Statistical analysis of properties of dwarf novae outbursts

Otulakowska-Hypka

Olech

Patterson

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…These secondary humps persisted during the quiescent state following the superoutburst, and the behavior is similar to the late stage of VW Hyi (subsection 3.22) and V344 Lyr (Kato et al 2012a;Wood et al 2011). Since SS UMi is considered to have a high mass-transfer rate comparable to ER UMa stars (Kato et al 2000a;Olech et al 2006), these secondary humps are possibly "traditional" late superhumps arising from the stream impact point. The signal became less convincing after the next normal outburst.…”

Section: Pu Ursae Majorismentioning

confidence: 76%

“…We observed the late stage of a superoutburst in 2012 March. As in Olech et al (2006), the the main peak of the superhump was already diminishing and the secondary maximum was developing. We list times of maxima of these humps in table 49.…”

Section: Pu Ursae Majorismentioning

confidence: 92%

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. IV: The Fourth Year (2011-2012)

Kato,

Hambsch,

Maehara

et al. 2012

Preprint

View full text Add to dashboard Cite

Continuing the project described by Kato et al. (2009), we collected times of superhump maxima for 86 SU UMa-type dwarf novae mainly observed during the 2011-2012 season. We confirmed the general trends recorded in our previous studies, such as the relation between period derivatives and orbital periods. There are some systems showing positive period derivatives despite the long orbital periods. We observed the 2011 outburst of the WZ Sge-type dwarf nova BW Scl, and recorded an O − C diagram similar to those of previously known WZ Sge-type dwarf novae. The WZ Sge-type dwarf nova OT J184228.1+483742 showed an unusual pattern of double outbursts composed of an outburst with early superhumps and one with ordinary superhumps. We propose an interpretation that a very small growth rate of the 3:1 resonance due to an extremely low mass-ratio led to a quenching of the superoutburst before the ordinary superhumps appeared. We systematically studied ER UMa-type dwarf novae and found that V1159 Ori showed positive superhumps similar to ER UMa in the 1990s. The recently recognized ER UMa-type object BK Lyn dominantly showed negative superhumps, and its behavior was very similar to the presentday state of ER UMa. The pattern of period variations in AM CVn-type objects were very similar to short-period hydrogen-rich SU UMa-type dwarf novae, making them helium analogue of hydrogen-rich SU UMa-type dwarf novae. SBS 1108+574, a peculiar hydrogen-rich dwarf nova below the period minimum, showed a very similar pattern of period variations to those of short-period SU UMa-type dwarf novae. The mass-ratio derived from the detected orbital period suggests that this secondary is a somewhat evolved star whose hydrogen envelope was mostly stripped during the mass-exchange. CC Scl, MASTER OT J072948.66+593824.4 and OT J173516.9+154708 showed only low-amplitude superhumps with complex profiles. These superhumps are likely a combination of closely separated two periods.

show abstract

“…We therefore restricted our O − C analysis to E ≤ 50. The situation may be similar to another longperiod system SS UMi (Olech et al 2006). The resultant P dot was −2.3(3.4) × 10 −5 .…”

Section: V728 Coronae Australismentioning

confidence: 77%

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae

Kato,

Imada,

Uemura

et al. 2009

Preprint

View full text Add to dashboard Cite

We systematically surveyed period variations of superhumps in SU UMa-type dwarf novae based on newly obtained data and past publications. In many systems, the evolution of superhump period are found to be composed of three distinct stages: early evolutionary stage with a longer superhump period, middle stage with systematically varying periods, final stage with a shorter, stable superhump period. During the middle stage, many systems with superhump periods less than 0.08 d show positive period derivatives. We present observational characteristics of these stages and greatly improved statistics. Contrary to the earlier claim, we found no clear evidence for variation of period derivatives between superoutburst of the same object. We present an interpretation that the lengthening of the superhump period is a result of outward propagation of the eccentricity wave and is limited by the radius near the tidal truncation. We interpret that late stage superhumps are rejuvenized excitation of 3:1 resonance when the superhumps in the outer disk is effectively quenched. The general behavior of period variation, particularly in systems with short orbital periods, appears to follow the scenario proposed in Kato et al. (2008). We also present an observational summary of WZ Sge-type dwarf novae. Many of WZ Sge-type dwarf novae showed long-enduring superhumps during the post-superoutburst stage having periods longer than those during the main superoutburst. The period derivatives in WZ Sge-type dwarf novae are found to be strongly correlated with the fractional superhump excess, or consequently, mass ratio. WZ Sge-type dwarf novae with a long-lasting rebrightening or with multiple rebrightenings tend to have smaller period derivatives and are excellent candidate for the systems around or after the period minimum of evolution of cataclysmic variables.

show abstract

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

Cited by 15 publications

References 26 publications

Statistical analysis of properties of dwarf novae outbursts

Statistical analysis of properties of dwarf novae outbursts

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. IV: The Fourth Year (2011-2012)

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae

Contact Info

Product

Resources

About