The X‐Ray Spectral Evolution of Classical Nova V1974 Cygni 1992: A Reanalysis of the<i>ROSAT</i>Data

Balman, Ş.; Krautter, J.; Öğelman, H.

doi:10.1086/305600

Cited by 103 publications

(184 citation statements)

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“…Generally in CNe this timescale is much longer than that observed in M31N 2007-12b (although Pietsch et al 2007, make the point that this might be ascribed in part to a selection effect). For example, in one of the best studied cases, the moderately fast CN V1974 Cyg, 511 days < t rem < 612 days (Balman et al 1998) with M WD ∼ 1 M (Hachisu & Kato 2006). From Starrfield et al (1991), t rem < 169 days implies M WD 1.3 M .…”

Section: Constraints From the X-ray Datamentioning

confidence: 99%

OPTICAL AND X-RAY OBSERVATIONS OF M31N 2007-12b: AN EXTRAGALACTIC RECURRENT NOVA WITH A DETECTED PROGENITOR?

Bode

Darnley

Shafter

et al. 2009

ApJ

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We report combined optical and X-ray observations of nova M31N 2007-12b. Optical spectroscopy obtained 5 days after the 2007 December outburst shows evidence of very high ejection velocities (FWHM Hα 4500 km s −1 ). In addition, Swift X-ray data show that M31N 2007-12b is associated with a Super-Soft Source (SSS) which appeared between 21 and 35 days post-outburst and turned off between then and day 169. Our analysis implies that M WD 1.3 M in this system. The optical light curve, spectrum, and X-ray behavior are consistent with those of a recurrent nova. Hubble Space Telescope observations of the pre-outburst location of M31N 2007-12b reveal the presence of a coincident stellar source with magnitude and color very similar to the Galactic recurrent nova RS Ophiuchi at quiescence, where the red giant secondary dominates the emission. We believe that this is the first occasion on which a nova progenitor system has been identified in M31. However, the greatest similarities of outburst optical spectrum and SSS behavior are with the supposed Galactic recurrent nova V2491 Cygni. A previously implied association of M31N 2007-12b with nova M31N 1969-08a is shown to be erroneous, and this has important lessons for future searches for recurrent novae in extragalactic systems. Overall, we show that suitable complementary X-ray and optical observations can be used not only to identify recurrent nova candidates in M31, but also to determine subtypes and important physical parameters of these systems. Prospects are therefore good for extending studies of recurrent novae into the Local Group with the potential to explore in more detail such important topics as their proposed link to Type Ia Supernovae.

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Section: Constraints From the X-ray Datamentioning

confidence: 99%

OPTICAL AND X-RAY OBSERVATIONS OF M31N 2007-12b: AN EXTRAGALACTIC RECURRENT NOVA WITH A DETECTED PROGENITOR?

Bode

Darnley

Shafter

et al. 2009

ApJ

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“…Within 1Y2 yr the nebula may have a rich line spectrum, emitting mostly below 1 keV (e.g., Ness et al 2003Ness et al , 2005. Of the novae discussed above, the time for the hard component of the X-ray emission to cool was about 6 months for the two fast novae ( Balman et al 1998;Mukai & Ishida 2001), but was longer (over 18 months) for slow novae with massive ejecta (Orio et al 1996;Greiner et al 2003), potentially exceeding the duration of the supersoft phase. However, the gradual decrease in temperature means that the duration of novae as >2 keV X-ray sources is effectively shorter than the total duration of novae as shell X-ray sources.…”

Section: Novae As X-ray Transientsmentioning

confidence: 99%

Novae as a Class of Transient X‐Ray Sources

Mukai

Orio

Valle

2008

ApJ

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Motivated by the recently discovered class of faint (10 34 Y10 35 ergs s À1 ) X-ray transients in the Galactic center region, we investigate the 2Y10 keV properties of classical and recurrent novae. Existing data are consistent with the idea that all classical novae are transient X-ray sources with durations of months to years and peak luminosities in the 10 34 Y10 35 ergs s À1 range. This makes classical novae a viable candidate class for the faint Galactic center transients. We estimate the rate of classical novae within a 15 0 radius region centered on the Galactic center (roughly the field of view of XMM-Newton observations centered on Sgr A*) to be $0.1 yr À1 . Therefore, it is plausible that some of the Galactic center transients that have been announced to date are unrecognized classical novae. The continuing monitoring of the Galactic center region carried out by Chandra and XMM-Newton may therefore provide a new method to detect classical novae in this crowded and obscured region, where optical surveys are not, and can never hope to be, effective. Therefore, X-ray monitoring may provide the best means of testing the completeness of the current understanding of the nova populations.

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“…The total energy emitted during all stages is ∼10 44 -10 46 erg. In addition to the soft component due to H-burning, shocks in the hot circumstellar material can produce hard X-ray emission * (e.g., Brecher et al 1977;Willson et al 1984;Ögelman et al 1987;O'Brien et al 1994;Balman et al 1998, and references therein). Even if there is no shock wave in the outburst, shocks may originate in interacting winds, or they may be due to interaction between ejecta and pre-existing material.…”

Section: The CV Two-qpo Diagrammentioning

confidence: 99%

X-rays from cataclysmic variables

Kuulkers

Norton

Schwope

et al. 2006

Compact Stellar X-Ray Sources

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IntroductionCataclysmic Variables * (CVs) are a distinct class of interacting binaries, transferring mass from a donor star to a degenerate accretor, a white dwarf (WD). In all observational determinations, and as is required by theory for stable mass transfer, the donor star is of lower mass than the accretor.The majority of CVs have orbital periods, P orb , between 75 min and 8 h (see Ritter & Kolb 2003) and consist of Roche Lobe-filling main sequence donors and WDs. These are WD analogues of the low-mass X-ray binaries (LMXBs; see Chapter 1). In the period range 8 h-3 d the donors must have larger radii than dwarfs in order to fill their Roche Lobes and are therefore evolved subgiants. A few CVs are found with P orb ∼200 d, which require giant donors for them to be Lobe-filling. The absence of evolved CVs with periods ∼3 to ∼200 d is connected with the dynamical instability that results from an initial donor that had a mass larger than about 67% of that of the WD; such binaries will have experienced rapid mass transfer and shortened their periods during a common envelope phase. Beyond P orb ∼200 d, mass-transferring systems also exist. These constitute the symbiotic binaries (SBs) and are in general not Roche Lobe-filling, but instead consist of a WD orbiting in the wind of a supergiant, and are thus analogues of the high-mass X-ray binaries (see Chapter 1).At the short end of the period range a different kind of CV exists, i.e., in which the mass losing donors are themselves WDs; they are entirely deficient in hydrogen. These helium-transferring CVs are known, after the type star, as AM CVn stars and are observed to have P orb from 60 min down to at least as short as 10 min. They have evolved by passage through two common envelope phases, which leaves the cores of both of the component stars exposed.The CVs are divided into subtypes. These were originally based entirely on the behaviour seen in long-term optical light curves, but to this are now added more subtle parameters such as the presence of polarisation. In essence, a CV's gross behaviour is determined by the rate of mass transfer from the donor,Ṁ donor , and * See Hack & La Dous (1993) and Warner (1995) for comprehensive overviews.

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The X‐Ray Spectral Evolution of Classical Nova V1974 Cygni 1992: A Reanalysis of theROSATData

Cited by 103 publications

References 55 publications

OPTICAL AND X-RAY OBSERVATIONS OF M31N 2007-12b: AN EXTRAGALACTIC RECURRENT NOVA WITH A DETECTED PROGENITOR?

OPTICAL AND X-RAY OBSERVATIONS OF M31N 2007-12b: AN EXTRAGALACTIC RECURRENT NOVA WITH A DETECTED PROGENITOR?

Novae as a Class of Transient X‐Ray Sources

X-rays from cataclysmic variables

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