The 1992 outburst of the SU Ursae Majoris-type dwarf nova HV Virginis

Leibowitz, E. M.; Mendelson, Haim; Bruch, A.; Duerbeck, H. W.; Seitter, W. C.; Richter, G. A.

doi:10.1086/173689

Cited by 31 publications

(22 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Although these modulations were detected independently by different groups Mendelson et al 1992;Leibowitz et al 1994 and our group), the distinction of these modulations from (ordinary) superhumps should await yet another object. Our result of HV Vir in 1992 was published in Kato et al (2001) following modern interpretation.…”

Section: Early Superhumpsmentioning

confidence: 60%

WZ Sge-type dwarf novae

Katô

2015

Publications of the Astronomical Society of Japan

161

View full text Add to dashboard Cite

We have summarized the current understanding and recently obtained findings about WZ Sge-type dwarf novae. We also reviewed the historical development of the understanding of these objects, provided the modern criteria, and reviewed the past research in relation to superhumps, early superhumps and the outburst mechanism. We regard that the presence of early superhumps (reflecting the 2:1 resonance) and long or multiple rebrightenings are the best distinguishing properties of WZ Sge-type dwarf novae. We provided the updated list of nearly 100 WZ Sge-type dwarf novae mainly based on the data obtained by the VSNET Collaboration up to Kato et al. (2015) and discussed the statistics. We could detect early superhumps with amplitude larger than 0.02 mag in 63% of the studied WZ Sge-type dwarf novae, which makes early superhumps a useful distinguishing feature for WZ Sge-type dwarf novae. Theoretical light curves of early superhumps generally appear to reproduce the existence of many low-amplitude objects, supporting the geometrical origin of early superhumps. Using the recently developed method of measuring mass ratios using developing phase of superhumps (stage A superhumps), we showed that there is a linear relation between the period variation of superhumps and the mass ratio in WZ Sge-type objects. By using this relation, we were able to draw an evolutionary picture of a large number of WZ Sge-type and identified the type of outburst to be an evolutionary sequence: type C → D → A → B → E, with some outliers for type-B objects. The duration of stage A (evolutionary phase) of superhumps is also well correlated with the estimated mass ratios. By using mass ratios from stage A superhumps and durarion of stage A, we have been able to identify best candidates for period bouncers.

show abstract

Section: Early Superhumpsmentioning

confidence: 60%

WZ Sge-type dwarf novae

Katô

2015

Publications of the Astronomical Society of Japan

161

View full text Add to dashboard Cite

show abstract

“…Further indication of the link comes from the quasi-periodic nature of the longer periodicity, which is a common characteristic of SHs periods (e.g. Patterson et al 1993a, Leibowitz et al 1994. This similarity to the SH phenomenon is quantitative as well.…”

Section: Superhump Interpretationmentioning

confidence: 93%

Permanent superhumps in nova V1974 Cygni (1992)

Retter

Leibowitz

Ofek

1997

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present results of 32 nights of CCD photometry of V1974 Cygni, from the years 1994 and 1995. We verify the presence of two distinct periodicities in the light curve: 0.0812585 day ≈ 1.95 hours and 0.0849767 d ≈ 2.04 hr. We establish that the shorter periodicity is the orbital period of the underlying binary system. The longer period oscillates with an average value of |Ṗ | ∼ 3 × 10 −7 -typical to permanent superhumps.The two periods obey the linear relation between the orbital and superhump periods that holds among members of the SU Ursae Majoris class of dwarf novae. A third periodicity of 0.083204 d ≈ 2.00 hr appeared in 1994 but not in 1995. It may be related to the recently discovered anti-superhump phenomenon. These results suggest a linkage between the classical nova V1974 Cyg and the SU UMa stars, and indicate the existence of an accretion disk and permanent superhumps in the system no later than 30 months after the nova outburst.From the precessing disk model of the superhump phenomenon we estimate that the mass ratio in the binary system is between 2.2 and 3.6. Combined with previous results this implies a white dwarf mass of 0.75-1.07 M ⊙ .

show abstract

“…Kato et al (1996);Patterson et al (1996);Nogami et al (1997a) ‡ Kato et al (2001b)Ishioka et al (2003);Leibowitz et al (1994).§ Ishioka et al (2002); Patterson et al (2002); R. Ishioka et al in preparation.§ Calculated from the periods of early superhumps and common superhumps except for WZ Sge.…”

mentioning

confidence: 99%

Superhumps and Repetitive Rebrightenings of the WZ Sge-Type Dwarf Nova, EG Cancri

Katô

Nogami

Matsumoto

et al. 2004

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

We report on time-resolved photometric observations of the WZ Sge-type dwarf nova, EG Cnc (Huruhata's variable), during its superoutburst in 1996-1997. EG Cnc, after the main superoutburst accompanied with development of superhumps typical of a WZ Sge-type dwarf nova, exhibited a series of six major rebrightenings. During these rebrightenings and the following long fading tail, EG Cnc persistently showed superhumps having a period equal to the superhump period observed during the main superoutburst. The persistent superhumps had a constant superhump flux with respect to the rebrightening phase. These findings suggest the superhumps observed during the rebrightening stage and the fading tail are a "remnant" of usual superhumps, and are not newly triggered by rebrightenings. By comparison with the 1977 outburst of this object and outbursts of other WZ Sge-type dwarf novae, we propose an activity sequence of WZ Sge-type superoutbursts, in which the current outburst of EG Cnc is placed between a single-rebrightening event and distinct outbursts separated by a dip. The post-superoutburst behavior of WZ Sge-type dwarf novae can be understood in the presence of considerable amount of remnant matter behind the cooling front in the outer accretion disk, even after the main superoutburst. We consider the premature quenching of the hot state due to the weak tidal effect under the extreme mass ratio of the WZ Sge-type binary is responsible for the origin of the remnant mass.

show abstract

The 1992 outburst of the SU Ursae Majoris-type dwarf nova HV Virginis

Cited by 31 publications

References 0 publications

WZ Sge-type dwarf novae

WZ Sge-type dwarf novae

Permanent superhumps in nova V1974 Cygni (1992)

Superhumps and Repetitive Rebrightenings of the WZ Sge-Type Dwarf Nova, EG Cancri

Contact Info

Product

Resources

About