High-speed photometry of the recurrent nova IM Normae

Woudt, P. A.; Warner, Brian D.

doi:10.1046/j.1365-8711.2003.06666.x

Cited by 19 publications

(19 citation statements)

References 14 publications

(17 reference statements)

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“…The decay time t 3 10 d following the equation t 3 2.75 t 0.88 2 from Warner (1995) gives a rough white dwarf mass estimate of 1.16 M (mass ratio <0.2). Woudt & Warner (2003b) interpreted the deep eclipse as obscuration of the disc and did not detect any periodicity near the orbital period in the period analysis. Therefore, following the tidal instability model, it is again probable that the disc is not fully developed up to 3:1 resonance radius 3 years after the outburst; however, the authors argue that the disc radius is 47% of the orbital separation.…”

Section: Searching For Superhumps In Other Nova Remnantsmentioning

confidence: 89%

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Nova V5116 Sagittarii and searching for superhumps in nova remnants

Dobrotka¹,

Retter²,

Liu³

2007

A&A

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Aims. We present the period analysis of unfiltered photometric observations of V5116 Sgr (Nova Sgr 2005 #2) and search for superhump candidates in novae remnants. Methods. The PDM method for period analysis was used. The masses of the novae componets we are estimated from the secondary mass -orbital period and primary mass -decline time relations. Results. We find that 13 nights of V5116 Sgr observations in the year 2006 are modulated with a period of 0.1238 ± 0.0001 d (2.9712 ± 0.0024 h). Following the shape of the phased light curves and no apparent change in the value of the periodicity in different subsamples of the data, we interpreted the period as orbital in nature. The binary system then falls within the period gap of the orbital period distribution of cataclysmic variables. From the maximum magnitude -rate of decline relation, we estimated a maximum absolute visual magnitude of M Vmax = −8.85 ± 0.04 mag using the measured value of decline t 2 = 6.5 ± 1.0 d. The mass-period relation for cataclysmic variables yields a secondary mass estimate of about 0.26 ± 0.05 M . We propose that V5116 Sgr is a high inclination system showing an irradiation effect of the secondary star. No fully developed accretion disc up to the tidal radius with the value lower than 3.5 × 10 10 cm is probable. The mass ratio was estimated in a few novae and the presence or absence of superhumps in these systems was compared with the mass ratio limit for superhumps of about 0.35. We find that, in the majority of novae with expected superhumps, this variability has not been found yet. Therefore, more observations of these systems is encouraged.

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Section: Searching For Superhumps In Other Nova Remnantsmentioning

confidence: 89%

“…A comparison to two novae within the period gap IM Nor and DD Cir with present irradiation effect (Woudt & Warner 2003b, c) can be made. The light curve of V5116 Sgr is different from those of IM Nor and DD Cir but similar to V2540 Oph.…”

Section: Short-term Variations Of V5116 Sgrmentioning

confidence: 99%

Nova V5116 Sagittarii and searching for superhumps in nova remnants

Dobrotka¹,

Retter²,

Liu³

2007

A&A

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“…have P orb > 100 days. The properties of IM Nor, which was not recognised as a recurrent nova when the review by Warner (1995) was published, are given by Kato et al (2002) and Woudt & Warner (2003). Schaefer (2010) recently proposed to divide the recurrent novae into two groups: i.e.…”

Section: Classification Of CI Aqlmentioning

confidence: 99%

Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

Iijima¹

2012

A&A

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High-and low-resolution optical spectra of CI Aql were obtained during the outburst in 2000. Multiple absorption components of H I and Fe II lines were detected at the early decline stage. Their radial velocities were roughly −2500 km s −1 , −2200 km s −1 , −1700 km s −1 , and −1400 km s −1 , among which only the last components were likely still accelerating during the early decline stage. Prominent emission lines of [O III] and [N II] appeared about one month after light maximum. The duration of the nebular stage, however, was only one month and a few weeks. The ejected gas shells seem to have started to shrink about 70 days after light maximum. The amount of interstellar extinction is estimated to be E(B − V) = 0.92 ± 0.15 from the equivalent widths of the diffuse interstellar absorption bands. The helium abundance in the ejecta is estimated to be N(He) = 0.19 ± 0.05 and the mass of the ejecta to be about 2 × 10 −6 M . This object has been classified as a U Sco type recurrent nova, but its spectral evolution during the outburst resembled those of T Pyx type recurrent novae. It is doubtful whether the peak of m V 9 mag on 2000 May 5 was the true light maximum or an earlier brighter peak had been overlooked, because the spectral data suggest that the ejections of gas shells occurred prior to the discovery of the outburst on 2000 April 28.

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“…It was detected as a hard X-ray source 6 months after the 2002 outburst [12]. [24] found its P orb to be 2.46h which places IM Nor in the middle of the CV period gap, an interval in the distribution of CV orbital periods between 2 hr and 3 hr where very few CVs are found.…”

Section: Im Norma (Nova Nor 1920)mentioning

confidence: 98%

The Hot Components in the Recurrent Novae T Pyxidis, IM Norma, CI Aquilae and in the Dwarf Nova U Geminorum

Sion¹,

Godon²

2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

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We report on the latest results from Hubble Space Telescope (HST) far ultraviolet spectroscopy with the Cosmic Object Spectrograph (COS), of the short orbital period recurrent novae (RNe) T Pyxidis, IM Norma (the first ever FUV spectrum of this RN) and CI Aquilae, the only known recurrent novae with main sequence donors and orbital periods less than a day. The last two HST COS spectra we obtained in October, 2016 and June, 2016, reveal that the accretion rate of T Pyx has declined by 20% below its quiescent continuum flux level recorded by the IUE following the 1966 outburst, an indication that the system might not have yet reached its (new) quiescent state. Recent HST COS Spectroscopy of the cooling of the white dwarf in the prototypical dwarf nova U Geminorum is also discussed with a focus on the chemical abundances in the white dwarf photosphere.

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High-speed photometry of the recurrent nova IM Normae

Cited by 19 publications

References 14 publications

Nova V5116 Sagittarii and searching for superhumps in nova remnants

Nova V5116 Sagittarii and searching for superhumps in nova remnants

Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

The Hot Components in the Recurrent Novae T Pyxidis, IM Norma, CI Aquilae and in the Dwarf Nova U Geminorum

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