Envelope models for the supersoft X-ray emission of V1974 Cyg

Sala, G.; Hernanz, M.

doi:10.1051/0004-6361:20042587

Cited by 17 publications

(20 citation statements)

References 28 publications

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“…They suggested the WD mass of M M 1.15 WD   . Sala & Hernanz (2005) calculated static sequences of hydrogen shellburning and compared them with the evolutional speed of post-wind phase for V1974Cyg. They suggested that the WD mass is M 0.9  for 50% mixing of a solar composition envelope with an ONe core (i.e., X 0.35…”

Section: Comparison With Previous Resultsmentioning

confidence: 99%

Light-Curve Analysis of Neon Novae

Hachisu

Kato

2015

ApJ

145

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We analyzed light curves of five neon novae, QUVul, V351Pup, V382Vel, V693CrA, and V1974Cyg, and determined their white dwarf (WD) masses and distance moduli on the basis of theoretical light curves composed of free-free and photospheric emission. For QUVul, we obtained a distance of d∼2.4 kpc, reddening of E (B−V)∼0. -M 1.1  . In QUVul, photospheric emission contributes 0.4-0.8 mag at most to the optical light curve compared with freefree emission only. In V351Pup and V1974Cyg, photospheric emission contributes very little (0.2-0.4 mag at most) to the optical light curve. In V382Vel and V693CrA, free-free emission dominates the continuum spectra, and photospheric emission does not contribute to the optical magnitudes. We also discuss the maximum magnitude versus rate of decline relation for these novae based on the universal decline law.

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Section: Comparison With Previous Resultsmentioning

confidence: 99%

Light-Curve Analysis of Neon Novae

Hachisu

Kato

2015

ApJ

145

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“…The duration of the SSS phase is inversely related to the WD mass while the time of appearance of the SSS is determined by the mass ejected in the outburst and the ejection velocity. Models of the post-outburst WD envelope show that steady H-burning can only occur for enPartly based on observations with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and NASA Corresponding author: wnp@mpe.mpg.de velope masses smaller than ∼ 10 −5 M (Sala & Hernanz 2005b;Tuchman & Truran 1998), and the observed evolution of the SSS in V1974 Cyg has been successfully modelled by an envelope of ∼ 2×10 −6 M (Sala & Hernanz 2005a). WD envelope models show that the duration of the SSS state also depends on the metallicity of the envelope, so the monitoring of the SSS states of CNe provides constraints also on the chemical composition of the post-outburst envelope.…”

Section: Introductionmentioning

confidence: 99%

X‐ray emission from optical novae in M 31

Pietsch

2010

Astron Nachr

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The first supersoft source (SSS) identification with an optical nova in M 31 was based on ROSAT observations. Twenty additional X-ray counterparts (mostly identified as SSS by their hardness ratios) were detected using archival ROSAT, XMM-Newton and Chandra observations obtained before July 2002. Based on these results optical novae seem to constitute the major class of SSS in M 31. An analysis of archival Chandra HRC-I and ACIS-I observations obtained from July 2004 to February 2005 demonstrated that M 31 nova SSS states lasted from months to about 10 years. Several novae showed short X-ray outbursts starting within 50 d after the optical outburst and lasting only two to three months. The fraction of novae detected in soft X-rays within a year after the optical outburst was more than 30 %. Ongoing optical nova monitoring programs, optical spectral follow-up and an up-to-date nova catalogue are essential for the X-ray work. Re-analysis of archival nova data to improve positions and find additional nova candidates are urgently needed for secure recurrent nova identifications. Dedicated XMM-Newton/Chandra monitoring programs for X-ray emission from optical novae covering the centre area of M 31 continue to provide interesting new results (e.g. coherent 1105 s pulsations in the SSS counterpart of nova M31N 2007-12b). The SSS light curves of novae allow us -together with optical informationto estimate the mass of the white dwarf, of the ejecta and the burned mass in the outburst. Observations of the central area of M 31 allow us -in contrast to observations in the Galaxy -to monitor many novae simultaneously and proved to be prone to find many interesting SSS and nova types.

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“…The hot WD photosphere emits thermal radiation, in the super soft X-ray energy range, which can be observed once the ejecta becomes transparent enough. The duration of this super soft X-ray emitting phase depends on the nuclear burning timescale of the remaining H-rich envelope, i.e., on the amount of H-rich mass left after the explosion, which is related to the efficiency of mass-ejection during the nova explosion [28,29,34].…”

Section: Scenarios Of Nova Explosionsmentioning

confidence: 99%

V2487 Oph 1998: a post nova in an intermediate polar

Hernanz

2014

EPJ Web of Conferences

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Abstract. V2487 Oph (Nova Oph 1998) is a classical nova that exploded in 1998. XMM-Newton observations performed between 2 and 9 years after the explosion showed emission related to restablished accretion, and indicative of a magnetic white dwarf. The spectrum looks like that of a cataclysmic variable of the intermediate polar type. Anyway, we don't have yet a definitive confirmation of the intermediate polar character, through determination of spin and orbital periods. Although it is not the first nova exploding in a magnetic white dwarf, it is always challenging to reach explosive conditions when a standard accretion disk can't be formed, because of the magnetic field. In addition, V2487 Oph has been the first nova where a detection of X-rays -in the host binary system -has been reported prior to its eruption, in 1990 with the ROSAT satellite. V2487 Oph has been also detected in hard X-rays with INTEGRAL/IBIS and RXTE/PCA. Last but not least, V2487 Oph has been identified as a recurrent nova in 2008, since a prior eruption in 1900 has been reported through analysis of Harvard photographic plates. Therefore, it is expected to host a massive white dwarf and be a candidate for a type Ia supernova explosion. In a recent study of the progenitors of galactic novae, it has been emphasized that V2487 Oph is an important and interesting object, "intermediate" between the "standard" classical novae and other historical and well-known recurrent novae with shorter recurrence periods. It could be that in the end there's a continuous distribution of recurrence periods, instead of the common understanding up to now that "classical" and "recurrent" novae were quite apart (with recurrence periods of more than 10 4 years and less than 100 years -approximately -respectively). We present the results of our campaign of several observations with XMM-Newton. The consequences for the understanding of such a puzzling object are discussed.

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Envelope models for the supersoft X-ray emission of V1974 Cyg

Cited by 17 publications

References 28 publications

Light-Curve Analysis of Neon Novae

Light-Curve Analysis of Neon Novae

X‐ray emission from optical novae in M 31

V2487 Oph 1998: a post nova in an intermediate polar

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