Composition Influence upon the Core Mass–Luminosity Relation and Possible Implications for the Extinction Timescales of Classical Novae

Tuchman, Y.; Truran, J. W.

doi:10.1086/305978

Cited by 30 publications

(40 citation statements)

References 28 publications

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“…The burned masses are within the values expected from models of post-outburst novae with stable hydrogen burning envelopes (Sala & Hernanz 2005b;Tuchman & Truran 1998), while the ejected masses derived for M 31 novae are also in the ranges of the ejected masses predicted from hydrodynamical models of nova outbursts (José & Hernanz 1998). But without any information on the accreted mass and the degree of mixing of the accreted envelope with the degenerate core, we cannot draw a conclusion on the actual increase or decrease of the white dwarf mass and its long-term evolution.…”

Section: Discussionsupporting

confidence: 77%

X-ray monitoring of optical novae in M 31 from July 2004 to February 2005

Pietsch¹,

Haberl²,

Sala³

et al. 2007

A&A

116

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Context. Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. Aims. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. Methods. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. Results. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380 d after outburst. One nova is detected to turn on 50 d, another 200 d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50 d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. Conclusions. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (>30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.

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Section: Discussionsupporting

confidence: 77%

X-ray monitoring of optical novae in M 31 from July 2004 to February 2005

Pietsch¹,

Haberl²,

Sala³

et al. 2007

A&A

116

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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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“…In general, more massive WDs retain less accreted mass after the explosion, although this also depends on the accretion rate, and reach larger luminosities (Yaron et al 2005). Thus, the duration of the SSS state is inversely related to the mass of the WD (Sala & Hernanz 2005;Tuchman & Truran 1998). In turn, the transparency requirement mentioned above implies that the time of appearance of the SSS is determined by the fraction of mass ejected in the outburst (Hachisu & Kato 2006).…”

Section: Introductionmentioning

confidence: 99%

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Henze

Pietsch

Haberl

et al. 2009

A&A

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Context. Classical novae (CNe) have been found to represent the major class of supersoft X-ray sources (SSSs) in our neighbour galaxy M 31. Aims. We determine the properties and evolution of the two first SSSs ever discovered in the M 31 globular cluster (GC) system. Methods. We have used XMM-Newton, Chandra and Swift observations of the centre region of M 31 to discover both SSSs and to determine their X-ray light curves and spectra. We performed detailed analysis of XMM-Newton EPIC PN spectra of the source in Bol 111 (SS1) using blackbody and NLTE white dwarf (WD) atmosphere models. For the SSS in Bol 194 (SS2) we used optical monitoring data to search for an optical counterpart. Results. Both GC X-ray sources were classified as SSS. We identify SS1 with the CN M31N 2007-06b recently discovered in the M 31 GC Bol 111. For SS2 we did not find evidence for a recent nova outburst and can only provide useful constraints on the time of the outburst of a hypothetical nova. Conclusions. The only known CN in a M 31 GC can be identified with the first SSS found in a M 31 GC. We discuss the impact of our observations on the nova rate for the M 31 GC system.

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Composition Influence upon the Core Mass–Luminosity Relation and Possible Implications for the Extinction Timescales of Classical Novae

Cited by 30 publications

References 28 publications

X-ray monitoring of optical novae in M 31 from July 2004 to February 2005

X-ray monitoring of optical novae in M 31 from July 2004 to February 2005

X‐ray emission from optical novae in M 31

The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

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