The Hydrogen-Burning Turnoff of RS Ophiuchi (2006)

Hachisu, Izumi; Kato, Mariko; Kiyota, S.; Kubotera, Katsuaki; Maehara, Hiroyuki; Nakajima, Kazuhiro; Ishii, Yuko; Kamada, M.; Mizoguchi, Shigeru; Nishiyama, Shinji; Sumitomo, N.; Tanaka, K.; Yamanaka, Masahito; Sadakane, Kozo

doi:10.1086/509615

Cited by 55 publications

(59 citation statements)

References 27 publications

(38 reference statements)

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“…23 Could the optical/NUV light curve plateau presented in DHB16 be caused by the surviving disk being unveiled by the receding photosphere? A similar prediction was made for a number of Galactic RNe by Hachisu et al (2008).…”

Section: The Accretion Disksupporting

confidence: 67%

Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Photometry of the 2015 Eruption

Darnley

Hounsell

Godon

et al. 2017

ApJ

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The recurrent nova M31N 2008-12a experiences annual eruptions, contains a near-Chandrasekhar-mass white dwarf, and has the largest mass accretion rate in any nova system. In this paper, we present Hubble Space Telescope (HST) WFC3/UVIS photometry of the late decline of the 2015 eruption. We couple these new data with archival HST observations of the quiescent system and Keck spectroscopy of the 2014 eruption. The late-time photometry reveals a rapid decline to a minimum luminosity state, before a possible recovery/rebrightening in the run up to the next eruption. Comparison with accretion disk models supports the survival of the accretion disk during the eruptions, and uncovers a quiescent disk mass accretion rate of the order of --

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Section: The Accretion Disksupporting

confidence: 67%

Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Photometry of the 2015 Eruption

Darnley

Hounsell

Godon

et al. 2017

ApJ

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“…While the spectra of novae with longer SSS states have lower temperatures (M31N 2000-07a and M31N 1999-10a show a kT of about 30−35 eV), the novae with short SSS state seem to have significantly higher temperatures (M31N 2004-06a and M31N 2004-08a about 70−80 eV). This fits to the nova outburst behavior calculated by Hachisu & Kato (2006a) that was successfully applied to predict and model the X-ray light curve of the recurrent nova RS Oph (Hachisu & Kato 2006b;Hachisu et al 2006), V1974 Cyg , V693 CrA, V1668 Cyg, V351 Pup and OS And . In these models novae with lower mass WDs show longer lasting SSS states with lower temperatures, novae with higher mass WDs show shorter SSS states with higher temperatures.…”

Section: Discussionmentioning

confidence: 69%

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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“…SN 2006X andSN 2007on) are possible WD + RG systems (Patat et al 2007a;Voss & Nelemans 2008). In addition, some recurrent nova (belonging to WD + RG) are suggested to be the candidates of SNe Ia progenitors (Hachisu et al 1999b;Hachisu & Kato 2006;Hachisu et al 2007). In this paper, we even proposed that the prevalence of the WD + RG channel is why no hydrogen line was detected in nebular spectra of some SNe Ia, although the probability of its occurrence is low.…”

Section: Wd + Rg Systemmentioning

confidence: 74%

The envelope mass of red giant donors in type Ia supernova progenitors

Meng¹,

Yang²

2010

A&A

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Context. The single degenerate model is the most widely accepted progenitor model of type Ia supernovae (SNe Ia), in which a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from a main sequence or a slightly evolved star (WD +MS) or from a red giant star (WD + RG), to increase its mass and explodes when approaching the Chandrasekhar mass. The explosion ejecta may impact the envelope of and strip off some hydrogen-rich material from the companion. The stripped-off hydrogen-rich material may manifest itself by means of a hydrogen line in the nebular spectra of SNe Ia. However, no hydrogen line is detected in the nebular spectra. Aims. We compute the remaining amounts of hydrogen in red giant donors to see whether the conflict between theory and observations can be overcome. Methods. By considering the mass-stripping effect from an optically thick wind and the effect of thermally unstable disk, we systematically carried out binary evolution calculation for WD + MS and WD + RG systems. Results. Here, we focus on the evolution of WD + RG systems. We found that some donor stars at the time of the supernova explosion contain little hydrogen-rich material on top of the helium core (as low as 0.017 M ), which is smaller than the upper limit to the amount derived from observations of material stripped-off by explosion ejecta. Thus, no hydrogen line is expected in the nebular spectra of these SN Ia. We also derive the distributions of the envelope mass and the core mass of the companions from WD + RG channel at the moment of a supernova explosion by adopting a binary population synthesis approach. We rarely find a RG companion with a very low-mass envelope. Furthermore, our models imply that the remnant of the WD + RG channel emerging after the supernova explosion is a single low-mass white dwarf (0.15−0.30 M ). Conclusions. The absence of a hydrogen line in nebular spectra of SNe Ia provides support to the proposal that the WD + RG system is the progenitor of SNe Ia.

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The Hydrogen-Burning Turnoff of RS Ophiuchi (2006)

Cited by 55 publications

References 27 publications

Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Photometry of the 2015 Eruption

Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Photometry of the 2015 Eruption

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

The envelope mass of red giant donors in type Ia supernova progenitors

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