Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Kang, Tae W.; Retter, A.; Liu, Alex; Richards, Mercedes T.

doi:10.1086/505174

Cited by 17 publications

(35 citation statements)

References 47 publications

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“…In spite of the likely different origin of the optical emission observed by Kang et al (2006), they found a similar period to our main frequency, yielding 0.7047 ± 0.0009 mHz, which is consistent with our optical/UV measurements obtained with XMM–Newton OM on day 742. While their frequency is remarkably close to our main X‐ray frequency, the statistical uncertainty ranges indicate a significant difference from all our measurements (see Table 2), including the late observations up to 1286 d after outburst.…”

Section: Discussionsupporting

confidence: 91%

“…V4743 Sgr has a quiescent X‐ray emission source (Ness et al 2007a) that could resemble those typically observed in intermediate polars, where X‐ray emission originates from an accretion shock close to the white dwarf. In addition, Kang et al (2006) detected a similar frequency of 0.7047 ± 0.0009 mHz in optical observations which is likely associated with magnetically controlled accretion columns. The authors interpreted this frequency as the beating between the spin frequency of the white dwarf and the orbital modulation.…”

Section: Discussionmentioning

confidence: 66%

“…The count rate dropped from 44 counts per second to 0.6 within ∼6 ks and stayed low for the rest of the observation (Ness 2010). Kang et al (2006) presented CCD unfiltered optical photometry analyses from observations taken in 2003 and 2005. They detected a period of 6.7 h which was interpreted as the orbital period of the underlying binary system.…”

Section: Introductionmentioning

confidence: 99%

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Multifrequency nature of the 0.75 mHz feature in the X-ray light curves of the nova V4743 Sgr

Dobrotka¹,

Ness²

2010

Monthly Notices of the Royal Astronomical Society

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We present timing analyses of eight X‐ray light curves and one optical/UV light curve of the nova V4743 Sgr (2002) taken by Chandra and XMM–Newton on the following days after outburst: 50 (early hard emission phase), 180, 196, 302, 371, 526 [super soft source (SSS) phase], and 742 and 1286 (quiescent emission phase). We have studied the multifrequency nature and time evolution of the dominant peak at ∼0.75 mHz using the standard Lomb–Scargle method and a 2D sine fitting method. We found a double structure of the peak and its overtone for days 180 and 196. The two frequencies were closer together on day 196, suggesting that the difference between the two peaks is gradually decreasing. For the later observations, only a single frequency can be detected, which is likely due to the exposure times being shorter than the beat period between the two peaks, especially if they are moving closer together. The observations on days 742 and 1286 are long enough to detect two frequencies with the difference found for day 196, but we confidently find only a single frequency. We found significant changes in the oscillation frequency and amplitude. We have derived blackbody temperatures from the SSS spectra, and the evolution of changes in frequency and blackbody temperature suggests that the 0.75‐mHz peak was modulated by pulsations. Later, after nuclear burning had ceased, the signal stabilized at a single frequency, although the X‐ray frequency differs from the optical/UV frequency obtained consistently from the Optical Monitor onboard XMM–Newton and from ground‐based observations. We believe that the late frequency is the white dwarf rotation and that the ratio of spin/orbit period strongly supports that the system is an intermediate polar.

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Section: Discussionsupporting

confidence: 91%

Section: Discussionmentioning

confidence: 66%

Section: Introductionmentioning

confidence: 99%

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Multifrequency nature of the 0.75 mHz feature in the X-ray light curves of the nova V4743 Sgr

Dobrotka¹,

Ness²

2010

Monthly Notices of the Royal Astronomical Society

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“…A probable spin period of the white dwarf was detected ∼1 yr after the outburst in V4745 Sgr (Dobrotka et al 2006a), ∼2.75 yr in V4743 Sgr (Kang et al 2006b), and ∼15 months after the maximum in V1425 Aql . Several systems show superhumps as early as two and a half months after the outburst like V4633 Sgr (a spin period is another option in this case, Lipkin et al 2001) or two years after the outburst like V1974 Cyg (Retter et al 1997).…”

Section: Short-term Variations Of V5116 Sgrmentioning

confidence: 96%

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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“…This is the hallmark of magnetic systems, and this one property has been used to identify many systems as magnetic. For examples amongst novae, see RW UMi (Tamburini et al 2007), V4633 Sgr (Lipkin & Leibowitz 2008), V4745 Sgr (Dobrotka et al 2006), V4743 Sgr (Kang et al 2006), V697 Sco (Warner & Woudt 2002), and V1495 Aql . (But this is not a forcing argument, as there are other means to make non-orbital photometric periodicities, for example, superhumps.)…”

Section: Nonthermal Emissionmentioning

confidence: 99%

The 2011 Eruption of the Recurrent Nova T Pyxidis: The Discovery, the Pre-Eruption Rise, the Pre-Eruption Orbital Period, and the Reason for the Long Delay

Schaefer

Landolt

Linnolt

et al. 2013

ApJ

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We report the discovery by M. Linnolt on JD 2, 455,665.7931 (UT 2011 April 14.29) of the sixth eruption of the recurrent nova T Pyxidis. This discovery was made just as the initial fast rise was starting, so with fast notification and response by observers worldwide, the entire initial rise was covered (the first for any nova), and with high time resolution in three filters. The speed of the rise peaked at 9 mag day −1 , while the light curve is well fit over only the first two days by a model with a uniformly expanding sphere. We also report the discovery by R. Stubbings of a pre-eruption rise starting 18 days before the eruption, peaking 1.1 mag brighter than its long-time average, and then fading back toward quiescence 4 days before the eruption. This unique and mysterious behavior is only the fourth known (with V1500 Cyg, V533 Her, and T CrB) anticipatory rise closely spaced before a nova eruption. We present 19 timings of photometric minima from 1986 to 2011 February, where the orbital period is fast increasing with P /Ṗ = +313,000 yr. From 2008 to 2011, T Pyx had a small change in this rate of increase, so that the orbital period at the time of eruption was 0.07622950 ± 0.00000008 days. This strong and steady increase of the orbital period can only come from mass transfer, for which we calculate a rate of (1.7-3.5) × 10 −7 M yr −1 . We report 6116 magnitudes between 1890 and 2011, for an average B = 15.59 ± 0.01 from 1967 to 2011, which allows for an eruption in 2011 if the blue flux is nearly proportional to the accretion rate. The ultraviolet-optical-infrared spectral energy distribution is well fit by a power law with f ν ∝ ν 1.0 , although the narrow ultraviolet region has a tilt with a fit of f ν ∝ ν 1/3 . We prove that most of the T Pyx light is not coming from a disk, or any superposition of blackbodies, but rather is coming from some nonthermal source. We confirm the extinction measure from IUE with E(B − V ) = 0.25 ± 0.02 mag.

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Nova V4743 Sagittarii 2002: An Intermediate Polar Candidate

Cited by 17 publications

References 47 publications

Multifrequency nature of the 0.75 mHz feature in the X-ray light curves of the nova V4743 Sgr

Multifrequency nature of the 0.75 mHz feature in the X-ray light curves of the nova V4743 Sgr

Nova V5116 Sagittarii and searching for superhumps in nova remnants

The 2011 Eruption of the Recurrent Nova T Pyxidis: The Discovery, the Pre-Eruption Rise, the Pre-Eruption Orbital Period, and the Reason for the Long Delay

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