XMM-Newton observations of Nova LMC 2000

Greiner, J.; Orio, Marina; Schartel, N.

doi:10.1051/0004-6361:20030602

Cited by 28 publications

(35 citation statements)

References 30 publications

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“…Finally, we note that Greiner et al (2003) did not find T Pyx to be a supersoft X-ray source, and that T Pyx does not appear in NASA's HEASARC tool (a master compilation of EUV and X-ray databases).…”

Section: Neither a Supersoft X-ray Source Nor Assisted Suicidementioning

confidence: 75%

The secrets of T Pyxidis

Selvelli¹,

Cassatella²,

Gilmozzi

et al. 2008

A&A

114

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Aims. We compare the observed and theoretical parameters for the quiescent and outburst phases of the recurring nova T Pyx. Methods. IUE data were used to derive the disk luminosity and the mass accretion rate, and to exclude the presence of quasi-steady burning at the WD surface. XMM-NEWTON data were used to verify this conclusion.. These values were about twice as high in the pre-1966-outburst epoch. This allowed the first direct estimate of the total mass accreted before outburst, M accr =Ṁ pre−OB ·Δt, and its comparison with the critical ignition mass M ign . We found M accr and M ign to be in perfect agreement (with a value close to 5 × 10 −7 M ) for M 1 ∼ 1.37 M , which provides a confirmation of the thermonuclear runaway theory. The comparison of the observed parameters of the eruption phase, with the corresponding values in the grid of models by Yaron and collaborators, provides satisfactory agreement for values of M 1 close to 1.35 M and logṀ between −8.0 and −7.0, but the observed value of the decay time t 3 is higher than expected. The long duration of the optically thick phase during the recorded outbursts of T Pyx, a spectroscopic behavior typical of classical novae, and the persistence of P Cyg profiles, constrains the ejected mass M ign to within 10 −5 −10 −4 M . Therefore, T Pyx ejects far more material than it has accreted, and the mass of the white dwarf will not increase to the Chandrasekhar limit as generally believed in recurrent novae. A detailed study based on the UV data excludes the possibility that T Pyx belongs to the class of the supersoft X-ray sources, as has been postulated. XMM-NEWTON observations have revealed a weak, hard source and confirmed this interpretation.

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Section: Neither a Supersoft X-ray Source Nor Assisted Suicidementioning

confidence: 75%

The secrets of T Pyxidis

Selvelli¹,

Cassatella²,

Gilmozzi

et al. 2008

A&A

114

View full text Add to dashboard Cite

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“…The right-hand panel of Figure 8 plots the turn-off time against the FWHM velocity of Hα or Hβ near visual maximum. The dotted line is the relationship from Greiner, Orio & Schartel (2003), which was derived from only a small sample of novae. This larger sample from Swift does not really support the model; specifically, many of the slow novae have turned off more quickly than expected from the Greiner relation.…”

Section: Turn-on and -Off Times Of The Sssmentioning

confidence: 99%

Swift Observations of Novae

Page¹

2011

Proc. IAU

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Abstract. The rapid response capability of Swift, together with the daily planning of its observing schedule, make it an ideal mission for following novae in the X-ray and UV bands. A number of both classical and recurrent novae have been extensively monitored throughout their supersoft phase. We report findings from these observations, including the high-amplitude flux variation often seen at the start of the supersoft emission, the optical plateau sometimes seen for recurrent novae, the differing relationships between the X-ray and UV variability, and the turn-on and turn-off times of the supersoft emission for the Swift sample of novae.

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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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XMM-Newton observations of Nova LMC 2000

Cited by 28 publications

References 30 publications

The secrets of T Pyxidis

The secrets of T Pyxidis

Swift Observations of Novae

Novae as a Class of Transient X‐Ray Sources

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