Variability and multiperiodic oscillations in the X-ray light curve of the classical nova V4743 Sgr

Leibowitz, E. M.; Orio, Marina; González‐Riestra, R.; Lipkin, Y.; Ness, J. U.; Starrfield, S.; Still, M.; Tepedelenlioǧlu, E.

doi:10.1111/j.1365-2966.2006.10684.x

Cited by 25 publications

(56 citation statements)

References 23 publications

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“…The amplitude of the modulation is a little above 5%. This period is likely to be the spin period of the WD, like for the Galactic nova V4743 Sgr, another luminous SSS (Leibowitz et al 2006). The X-ray luminosity was above 10 38 erg s −1 after two months, with a WD atmospheric temperature 760,000 K (lower panel of Figure 10).…”

Section: Classical and Recurrent Novae As Sssmentioning

confidence: 95%

“…We do find this periodicity in most, but not in all the uninterrupted observations done in recent years. In some observations, especially in early 2008, also several other periods ranging from few minutes to 2 hr are measured, like in Nova V4743 Sgr (Leibowitz et al 2006). Detailed temporal analysis will be in a dedicated paper.…”

Section: R2-12 the Ongoing Fireworkmentioning

confidence: 99%

“…First of all, the classical or recurrent novae among them have a very characteristic X-ray and optical light curve. Often, they also exhibit variations on minute timescales, which are attributed to either the spin of the WD or to non-radial pulsations (e.g., Drake et al 2003;Leibowitz et al 2006;Nelson et al 2008). The variability of other SSS WD binaries in the MC has also already been well monitored.…”

Section: Introductionmentioning

confidence: 99%

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A Census of the Supersoft X-Ray Sources in M31

Orio¹,

Nelson²,

Bianchini³

et al. 2010

ApJ

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We examined X-ray, ultraviolet, and optical archival data of 89 supersoft X-ray sources (SSS) in M31. We studied the timescales of X-ray variability and searched UV and optical counterparts. Almost a third of the SSS are known classical or recurrent novae, and at least half of the others exhibit the same temporal behavior as post-outburst novae. Non-stellar objects among SSS seem to be rare: less than 10% of the classified SSS turned out to be supernova remnants, and only one source has been identified with an active galactic nucleus in the background. Not more than 20% of the SSS that are not coincident with observed novae are persistent or recurrent X-ray sources. A few of these long-lasting sources show characteristics in common with other SSS identified as white dwarf (WD) close binaries in the Magellanic Clouds and in the Galaxy, including variability on timescales of minutes, possibly indicating the spin period of a WD. Such objects are likely to be low-mass X-ray binaries with a massive WD. A third of the non-nova SSS are in regions of recent star formation, often at the position of an O or B star, and we suggest that they may be high-mass X-ray binaries. If these sources host a massive hydrogen-burning WD, as it seems likely, they may become Type Ia supernovae (SNe Ia), constituting the star formation dependent component of the SNe Ia rate.

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Section: Classical and Recurrent Novae As Sssmentioning

confidence: 95%

Section: R2-12 the Ongoing Fireworkmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Census of the Supersoft X-Ray Sources in M31

Orio¹,

Nelson²,

Bianchini³

et al. 2010

ApJ

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“…There are also several other IP candidates: V1425 Cyg, V533 Her and V842 Cen 3 , V4743 Sgr (Leibowitz et al 2006;Dobrotka & Ness 2010). Little is known how the magnetic field changes the nova evolution, it may really steer the path towards, or away from, a type Ia SN explosion in RNe.…”

Section: Discussionmentioning

confidence: 99%

SUZAKUOBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE

Zemko

Mukai

Orio

2015

ApJ

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We present Suzaku XIS observation of V2491 Cyg (Nova Cyg 2008 No. 2) obtained in quiescence, more than two years after the outburst. The nova was detected as a very luminous source in a wide spectral range from soft to hard X-rays. A very soft blackbody-like component peaking at 0.5 keV indicates that either we observe remaining, localized hydrogen burning on the surface of the white dwarf, or accretion onto a magnetized polar cap. In the second case, V2491 Cyg is a candidate "soft intermediate polar". We obtained the best fit for the X-ray spectra with several components: two of thermal plasma, a blackbody and a complex absorber. The later is typical of intermediate polars.The X-ray light-curve shows a modulation with a ∼38 min period. The amplitude of this modulation is strongly energy dependent and reaches maximum in the 0.8-2.0 keV range. We discuss the origin of the X-ray emission and pulsations, and the likelihood of the intermediate polar scenario.

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“…6.7 h and ∼ 1300 s; Leibowitz et al 2006;Dobrotka & Ness 2010), V5116 Sgr (2.97 h; Sala et al 2008), CSS 081007:030559+054715 (1.77 d; Osborne et al 2009) and KT Eri (35 s; Beardmore et al 2010).…”

Section: X-ray Variability Of Nova M31n 2006-04amentioning

confidence: 99%

X-ray monitoring of classical novae in the central region of M 31

Henze

Pietsch

Haberl

et al. 2010

A&A

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Context. Classical novae (CNe) have recently been reported to represent the major class of supersoft X-ray sources (SSSs) in the central region of our neighbour galaxy M 31. Aims. We carried out a dedicated monitoring of the M 31 central region with XMM-Newton and Chandra in order to find SSS counterparts of CNe, determine the duration of their SSS phase and derive physical outburst parameters. Methods. We systematically searched our data for X-ray counterparts of CNe and determined their X-ray light curves and spectral properties. Additionally, we determined luminosity upper limits for all novae from previous studies which are not detected anymore and for all CNe in our field of view with optical outbursts between May 2005 and March 2007. Results. We detected eight X-ray counterparts of CNe in M 31, four of which were not previously known. Seven sources can be classified as SSSs, one is a candidate SSS. Two SSSs are still visible more than nine years after the nova outburst, whereas two other nova counterparts show a short SSS phase of less than 150 days. Of the latter sources, M31N 2006-04a exhibits a short-time variable X-ray light curve with an apparent period of (1.6 ± 0.3) h. This periodicity could indicate the binary period of the system. There is no X-ray detection for 23 out of 25 CNe which were within the field of view of our observations and had their outburst from about one year before the start of the monitoring until its end. From the 14 SSS nova counterparts known from previous studies, ten are not detected anymore. Additionally, we found four SSSs in our XMM-Newton data without a nova counterpart, one of which is a new source. Conclusions. Out of eleven SSSs detected in our monitoring, seven are counterparts of CNe. We therefore confirm the earlier finding that CNe are the major class of SSSs in the central region of M 31. We use the measured SSS turn-on and turn-off times to estimate the mass ejected in the nova outburst and the mass burned on the white dwarf. Classical novae with short SSS phases seem to be an important contributor to the overall population.

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Variability and multiperiodic oscillations in the X-ray light curve of the classical nova V4743 Sgr

Cited by 25 publications

References 23 publications

A Census of the Supersoft X-Ray Sources in M31

A Census of the Supersoft X-Ray Sources in M31

SUZAKUOBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE

X-ray monitoring of classical novae in the central region of M 31

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