Permanent superhumps in nova V1974 Cygni (1992)

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

doi:10.1093/mnras/286.3.745

Cited by 58 publications

(71 citation statements)

References 25 publications

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“…8) is also evidence supporting the superhump interpretation (see, e.g., Fig. 5 of Retter et al 1997 and Fig. 4 of Patterson et al 1997).…”

Section: Discussionsupporting

confidence: 70%

Detection of superhumps in the Z Camelopardalis-type dwarf nova AT Cnc at standstill

Kozhevnikov

2004

A&A

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Abstract. We present results of our photometry of the Z Camelopardalis-type dwarf nova AT Cnc. The observational data were obtained during 13 nights in February and March 2003 when AT Cnc was in its long standstill. Two sets of our data reveal brightness variations with quasi-periods of (4.65 ± 0.02) and of (4.74 ± 0.02) h. The semiamplitude of these variations was observed in the range 5-9 mmag, showing changes from night to night. This signal varies in period and in phase on a time-scale of weeks, as is typical of superhumps. A comparison with the orbital period obtained by Nogami et al. (1999) from the radial velocity measurements of AT Cnc, which equals (4.826 ± 0.014) h, shows that this signal can be a negative superhump since the average period of brightness variations is approximately 3% shorter than the orbital period. These results make AT Cnc a permanent superhump system with a rather large orbital period and a large mass ratio. This is also the first detection of superhumps in a Z Camelopardalis-type system. In addition, we have found signs of an unstable signal with a period of about 2.3 h, which may represent the second harmonic of the 4.7-h signal or the second orbital sideband of the wobble frequency of the tilted precessing accretion disc. The average power spectrum of AT Cnc reveals a broad hump at frequencies in the range 0.4-0.7 mHz, which is evidence of quasiperiodic oscillations. The hump crest corresponds to a period of 1700-1800 s, which is remarkably close to 10% of the orbital period. This may indicate that this system contains a magnetic white dwarf creating the tilted accretion disc.

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“…8) is also evidence supporting the superhump interpretation (see, e.g., Fig. 5 of Retter et al 1997 and Fig. 4 of Patterson et al 1997).…”

Section: Discussionsupporting

confidence: 70%

Detection of superhumps in the Z Camelopardalis-type dwarf nova AT Cnc at standstill

Kozhevnikov

2004

A&A

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“…Such a large radius cannot be the radius of the white dwarf. In a nova outburst, the system returns to its normal dimension in a few weeks or months-much less than the 3 yr elapsed before our observations (Hauschildt et al 1997;Retter et al 1997;Retter 1999).…”

Section: Discussionmentioning

confidence: 70%

Interferometric Observations of V838 Monocerotis

Lane¹,

Retter²,

Thompson³

et al. 2005

ApJ

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We have used long-baseline near-IR interferometry to resolve the peculiar eruptive variable star V838 Mon and to provide the first direct measurement of its angular size. Assuming a uniform disk model for the emission, we derive an apparent angular diameter at the time of observations (2004 November-December) of 1.83 ‫ע‬ mas. For a nominal distance of kpc, this implies a linear radius of 1570 ‫ע‬ 400 R , . However, the 0.06 8 ‫ע‬ 2 data are somewhat better fitted by elliptical disk or binary component models, and we suggest that the emission may be strongly affected by ejecta from the outburst.

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“…He proposed that the accretion discs in IPs are fully destroyed in the nova outburst (contrary to other systems, for which observational evidence for early presence of the disc were founde.g. Leibowitz et al 1992;Retter et al 1997Retter et al , 1998. The reestablishment of the disc and the subsequent interaction with the magnetosphere of the primary white dwarf can be a violent process that may form strong winds in the inner part of the disc.…”

Section: A Comparison With Previous Modelsmentioning

confidence: 99%

Spectroscopic monitoring of the transition phase in nova V4745 Sgr

Csák¹,

Kiss

Retter

et al. 2004

A&A

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Abstract. We present a spectroscopic monitoring of the transient nova V4745 Sagittarii (Nova Sgr 2003 #1) covering ten months after its discovery. During this period the light curve showed a well expressed transient phase in the form of six rebrightenings, and the presented dataset is one of the best spectroscopic coverages of a classical nova during the transition phase. Low-and medium-resolution spectra revealed that the majority of spectral lines switched back to strong P-Cyg profiles during the mini-outbursts, similar to the spectra just after the major eruption. We interpret the observed phenomena as evidence for "echo-outbursts" resulting in episodes of secondary mass-ejections and propose that the transition phase in classical novae is driven by repetitive instabilities of the hydrogen shell burning on the surface of the white dwarf. From the available light curve data we estimate the absolute magnitude of the system of about −8. m 3 ± 0. m 5. All spectrophotometric evidence point toward a very low (E(B − V) < 0. m 1) interstellar reddening, leading to a rough distance estimate of V4745 Sgr (9 kpc < d < 19 kpc).

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Permanent superhumps in nova V1974 Cygni (1992)

Cited by 58 publications

References 25 publications

Detection of superhumps in the Z Camelopardalis-type dwarf nova AT Cnc at standstill

Detection of superhumps in the Z Camelopardalis-type dwarf nova AT Cnc at standstill

Interferometric Observations of V838 Monocerotis

Spectroscopic monitoring of the transition phase in nova V4745 Sgr

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