The presence of an accretion disk in the eclipsing binary system Nova Herculis 1991 three weeks after outburst

Leibowitz, E. M.; Mendelson, Haim; Mashal, E.; Prialnik, Dina; Seitter, W. C.

doi:10.1086/186275

Cited by 25 publications

(26 citation statements)

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“…They found that the eclipse depth of the 3.2 hr period was 10 times larger than in mid-2000. Both Leibowitz et al (1992) and Bos et al (2001) interpreted the phenomenon as an eclipse of the accretion disk by the secondary star. Similarly, we propose to explain the 6.7 hr variation in the light curve of V4743 Sgr as an eclipse of the accretion disk by the companion star or as a combination of an eclipse and aspect variations of the side of the comparison star, which is heated by the white dwarf (see also Balman et al 2006).…”

Section: Discussionmentioning

confidence: 99%

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Kang

Retter

Liu³

et al. 2006

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We present the results of 11 nights of CCD unfiltered photometry of V4743 Sgr (Nova Sgr 2002 No. 3) from 2003 and 2005. We find two periods of 0.2799 days (%6.7 hr) and 0.01642 days (%24 minutes) in the 2005 data. The long period is also present in the 2003 data, but only weak evidence of the shorter period is found in this year. The 24 minute period is somewhat longer than the 22 minute period that was detected from X-ray observations. We suggest that the 6.7 hr periodicity represents the orbital period of the underlying binary system and that the 24 minute period is the beat periodicity between the orbital period and the X-ray period, which is presumably the spin period of the white dwarf. Thus, V4743 Sgr should be classified as an intermediate polar (DQ Her star). About 6 months after the nova outburst, the optical light curve of V4743 Sgr seemed to show quasi-periodic oscillations, which are typical of the transient phase in classical novae. Therefore, our results support the previous suggestion that the transition phase in novae may be related to intermediate polars.

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Section: Discussionmentioning

confidence: 99%

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Kang

Retter

Liu³

et al. 2006

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“…Leibowitz et al (1992) showed that a disc may be present in post novae already a few days after the explosion, and, hence, it seems plausible that the L 1 point is efficiently shielded in most, if not all nonmagnetic post novae. The only way to increase the mass transfer rate by irradiation on a short timescale even in the case of disc shielding is to assume meridional circulations which transport energy from the illuminated regions to the L 1 -region (Sarna 1990;Kirbiyik & Smith 1976;Kippenhahn & Thomas 1979;Meyer & Meyer-Hofmeister 1983).…”

Section: Discussionmentioning

confidence: 99%

Irradiated accretion discs in post novae

Schreiber

Gänsicke

2001

A&A

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Abstract. We derive approximations for theṀ − Σ relation (the so-called S-curves) of irradiated accretion discs from detailed vertical structure calculations. Using these approximations, we simulate the time-dependent behaviour of irradiated accretion discs in dwarf novae and post novae. Our calculations show, in agreement with Hameury et al. (1999), that irradiation of the accretion disc should cause small "echo" outbursts immediately following normal outbursts -which contrasts with the observed dwarf nova light curves. In addition, we calculate light curves of post nova systems where the accretion disc is strongly irradiated by the hot white dwarf. We find that the visual brightness of post novae gradually decreases after the nova explosion as a result of the decreasing disc irradiation from the continuously cooling white dwarf. The rate of decline that we derive is in good agreement with the observations. While we cannot exclude that additional effects may contribute to the observed fading of post novae, e.g., a slow decrease of the accretion rate, our calculations show that irradiation from the cooling white dwarf plays an important rôle in the post nova evolution.

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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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The presence of an accretion disk in the eclipsing binary system Nova Herculis 1991 three weeks after outburst

Cited by 25 publications

References 0 publications

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Irradiated accretion discs in post novae

Spectroscopic monitoring of the transition phase in nova V4745 Sgr

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