Permanent Superhumps in Nova V1974 Cygni 1992

Retter, A.; Leibowitz, E. M.; Ofek, E. O.

doi:10.1007/978-94-015-8941-3_23

Cited by 3 publications

(5 citation statements)

References 7 publications

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“…during 1995 and 1996, as well as other features of the optical LC of the nova discussed in Retter et al (1997), argue against the magnetic interpretation for the longer period, and for the PSH one, which we adopt in this letter.…”

Section: Superhumps In Classical Nova Systemsmentioning

confidence: 53%

“…Photometric observations of V1974 Cyg (N. Cyg 1992) revealed two periodic oscillations in the LC of the star (Retter, Ofek & Leibowitz 1995). While there is an overall agreement that the shorter is the orbital period of the binary system, two interpretations for the nature of the second period, which is about 5% larger than the orbital one, have been suggested.…”

Section: Superhumps In Classical Nova Systemsmentioning

confidence: 99%

“…Semeniuk et al (1995) and Olech et al (1996), argued that it is the spin period of a rotating WD. Retter, Leibowitz & Ofek (1997) and Skillman et al (1997) proposed, on the other hand, that the longer period is that of PSH oscillations. We think that the increase of this period (1996), showing the location on the (Orbital Period, Ṁ ) plane of four major groups of CVs: UG=U Geminorum, SU UMa, PSH=permanent superhumps and NL=nova like variables.…”

Section: Superhumps In Classical Nova Systemsmentioning

confidence: 99%

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Predicting the future of superhumps in classical nova systems

Retter

Leibowitz

1998

Monthly Notices of the Royal Astronomical Society

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Oscillations observed in the light curve of Nova V1974 Cygni 1992 since the summer of 1994 have been interpreted as permanent superhumps. From simple calculations based on the tidal disc instability model of Osaki, and assuming that the accretion disc is the dominant optical source in the binary system, we predict that the nova will evolve to become an SU UMa system as its brightness declines from its present value by another 2–3 mag. Linear extrapolation of its current rate of fading (in magnitude units) puts the time of this phase transition within the next 2–4 yr. Alternatively, the brightness decline will stop before the nova reaches that level, and the system will continue to show permanent superhumps in its light curve. It will then be similar to two other old novae, V603 Aql and CP Pup, which still display the permanent superhump phenomenon 80 and 56 yr, respectively, after their eruptions. We suggest that non‐magnetic novae with short orbital periods could be progenitors of permanent superhump systems.

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Section: Superhumps In Classical Nova Systemsmentioning

confidence: 53%

Section: Superhumps In Classical Nova Systemsmentioning

confidence: 99%

Section: Superhumps In Classical Nova Systemsmentioning

confidence: 99%

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Predicting the future of superhumps in classical nova systems

Retter

Leibowitz

1998

Monthly Notices of the Royal Astronomical Society

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“…Patterson et al (1995) observed the superhumps in the SU UMa system V1159 Orionis to persist well after superoutburst had ended. Modulations tentatively identified as superhumps have also been observed in several other short period cataclysmic variables (see Patterson & Richman 1991, Retter, Leibowitz & Ofek 1997) that don't exhibit classic dwarf novae activity.…”

Section: Superhumpsmentioning

confidence: 84%

Simulations of superhumps and superoutbursts

Murray

1998

Monthly Notices of the Royal Astronomical Society

106

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We numerically study the tidal instability of accretion discs in close binary systems using a two-dimensional SPH code. We find that the precession rate of tidally unstable, eccentric discs does not only depend upon the binary mass ratio q. Although the (prograde) disc precession rate increases with the strength of the tidal potential, it also increases with the shear viscosity. Increasing the disc temperature has a retrograde impact upon the precession rate. We find that motion relative to the binary potential results in superhump-like, periodic luminosity variations in the outer reaches of an eccentric disc. The nature and location of the luminosity modulation is a function of the shear viscosity, nu. Light curves most similar to observations are obtained for nu values appropriate for a dwarf nova in outburst. We investigate the thermal-tidal instability model for superoutburst. A dwarf nova outburst is simulated by instantaneously increasing nu, which causes a rapid radial expansion of the disc. Should the disc encounter the 3:1 eccentric inner Lindblad resonance and become tidally unstable, then tidal torques become much more efficient at removing angular momentum from the disc. The disc then shrinks and mass flux through the disc increases. The resulting increase in disc luminosity is found to be consistent with the excess luminosity of a superoutburst.Comment: 12 pages, 14 encapsulated postscipt figures, accepted by MNRA

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“…The two periods obey exactly the relation that holds between the orbital and superhump periods in the SU UMa members. (Stolz & Schoembs 1981, 1984Retter et al 1995, Retter, Leibowitz & Ofek 1996 3. We establish the coherence of the shorter periodicity, and hence the likelihood that it is the orbital period of the binary system.…”

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confidence: 99%

Photometric Evidence for the Presence of An Accretion Disk and for a Superhump - Like Phenomenon in the Classical Nova V1974 Cygni 1992

Retter

Leibowitz

Ofek

1997

International Astronomical Union Colloquium

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Abstract. The light curve of V1974 Cyg shows two distinct periodicities. The shorter periodicity is clearly the orbital period of the binary system. We show that the longer variation has similar features to permanent superhumps. This result indicates the existence of an accretion disk in the system no later than 30 months after the nova outburst. We used the precessing disk model of the superhump phenomenon and previous results in order to estimate that the white dwarf mass is at the range 0.75 -1.07 M 0 .

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Permanent Superhumps in Nova V1974 Cygni 1992

Cited by 3 publications

References 7 publications

Predicting the future of superhumps in classical nova systems

Predicting the future of superhumps in classical nova systems

Simulations of superhumps and superoutbursts

Photometric Evidence for the Presence of An Accretion Disk and for a Superhump - Like Phenomenon in the Classical Nova V1974 Cygni 1992

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