A remarkable recurrent nova in M 31: The predicted 2014 outburst in X-rays with<i>Swift</i>

Henze, M.; Ness, J. U.; Darnley, M. J.; Bode, M. F.; Williams, S. C.; Shafter, A. W.; Sala, G.; Kato, Mariko; Hachisu, Izumi; Hernanz, M.

doi:10.1051/0004-6361/201526028

Cited by 34 publications

(49 citation statements)

References 46 publications

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“…This prediction assumes a similar luminosity and spectrum for the X-ray flash and the SSS phase (see Fig. 1 and compare Henze et al 2015a;Kato et al 2015).…”

Section: Resultsmentioning

confidence: 96%

“…This means that the evolution time from C to D in Figure 1 was longer than eight days, and the optical/UV bright phase, from D to E, lasted about 5.5 days (Darnley et al 2015;Henze et al 2015a). Darnley et al (2015) pointed out that M31N 2008-12a showed slow rise to the optical peak magnitude in the 2014 outburst.…”

Section: Slow Evolution After X-ray Flashmentioning

confidence: 99%

“…We carried out a coordinated, very high-cadence observing campaign with the Swift satellite (Gehrels et al 2004) to detect the X-ray flash during the 2015 outburst of the recurrent nova M31N 2008-12a (Darnley et al 2014(Darnley et al , 2015Henze et al 2014aHenze et al , 2015aTang et al 2014). This is the ideal object to detect X-ray flashes because its recurrence period is as short as a year, possibly even half a year (Henze et al 2015b).…”

Section: Introductionmentioning

confidence: 99%

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X-RAY FLASHES IN RECURRENT NOVAE: M31N 2008-12a AND THE IMPLICATIONS OF THE SWIFT NONDETECTION

Kato

Saio

Henze

et al. 2016

ApJ

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Models of nova outbursts suggest that an X-ray flash should occur just after hydrogen ignition. However, this X-ray flash has never been observationally confirmed. We present four theoretical light curves of the X-ray flash for two very massive white dwarfs (WDs) of 1.380 and 1.385 M ⊙ and for two recurrence periods of 0.5 and 1 years. The duration of the X-ray flash is shorter for a more massive WD and for a longer recurrence period. The shortest duration of 14 hours (0.6 days) among the four cases is obtained for the 1.385 M ⊙ WD with one year recurrence period. In general, a nova explosion is relatively weak for a very short recurrence period, which results in a rather slow evolution toward the optical peak. This slow timescale and the predictability of very short recurrence period novae give us a chance to observe X-ray flashes of recurrent novae. In this context, we report the first attempt, using the Swift observatory, to detect an X-ray flash of the recurrent nova M31N 2008-12a (0.5 or 1 year recurrence period), which resulted in the non-detection of X-ray emission during the period of 8 days before the optical detection. We discuss the impact of these observations on nova outburst theory. The X-ray flash is one of the last frontiers of nova studies and its detection is essentially important to understand the pre-optical-maximum phase. We encourage further observations.

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“…This prediction assumes a similar luminosity and spectrum for the X-ray flash and the SSS phase (see Fig. 1 and compare Henze et al 2015a;Kato et al 2015).…”

Section: Resultsmentioning

confidence: 96%

Section: Slow Evolution After X-ray Flashmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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X-RAY FLASHES IN RECURRENT NOVAE: M31N 2008-12a AND THE IMPLICATIONS OF THE SWIFT NONDETECTION

Kato

Saio

Henze

et al. 2016

ApJ

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“…12a. Kato et al (2015) estimated the WD mass of M31N 2008-12a to be 1.38 M ☉ from the SSS duration that lasts about 8 days (Henze et al 2014(Henze et al , 2015Darnley et al 2016a). In the present paper, we do not consider the optical light curves because the relation between the optical brightness and wind mass-loss rate in recurrent novae is uncertain, which remains to be a subject for future work.…”

Section: 38 M E Modelmentioning

confidence: 99%

A Self-consistent Model for a Full Cycle of Recurrent Novae—Wind Mass-loss Rate and X-Ray Luminosity

Kato

Saio

Hachisu

2017

ApJ

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An unexpectedly slow evolution in the pre-optical-maximum phase was suggested in the very short recurrence period of nova M31N 2008-12a. To obtain reasonable nova light curves we have improved our calculation method by consistently combining optically thick wind solutions of hydrogen-rich envelopes with white dwarf (WD) structures calculated by a Henyey-type evolution code. The wind mass-loss rate is properly determined with high accuracy. We have calculated light curve models for 1.2M e and 1.38 M e WDs with mass accretion rates corresponding to recurrence periods of 10 yr and 1 yr, respectively. The outburst lasts 590/29 days, in which the pre-optical-maximum phase is 82/16 days, for 1.2/1.38 M e , respectively. Optically thick winds start at the end of the X-ray flash and cease at the beginning of the supersoft X-ray phase. We also present supersoft X-ray light curves including a prompt X-ray flash and later supersoft X-ray phase.

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“…(1) White et al (1995), (2) Henze et al (2015a), (3) Williams et al (2004), (4) Nishiyama & Kabashima (2008), (5) Tang et al (2014), (6) Korotkiy & Elenin (2011), (7) Barsukova et al (2011), (8) Darnley et al (2015e), (9) Nishiyama & Kabashima (2012), (10) Shafter et al (2012), (11) Henze et al (2014a), (12) Tang et al (2013), (13) Darnley et al (2014b), (14)this paper, (15) Henze et al (2015d), (16) Darnley et al (2015b), (17) Darnley et al (2015d), (18) Henze et al (2015c). Henze et al (2014a;hereafter, HND14) and Tang et al (2014;hereafter, TBW14) independently uncovered earlier eruptions from 1992, 1993, and 2001.…”

Section: A Remarkable Rnmentioning

confidence: 99%

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

Darnley

Henze

Bode

et al. 2016

ApJ

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The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of =  P 351 13 rec days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground-and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swiftobservatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28±0.12 UT. The 2013-2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities ∼13,000 km s −1 ,

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A remarkable recurrent nova in M 31: The predicted 2014 outburst in X-rays withSwift

Cited by 34 publications

References 46 publications

X-RAY FLASHES IN RECURRENT NOVAE: M31N 2008-12a AND THE IMPLICATIONS OF THE SWIFT NONDETECTION

X-RAY FLASHES IN RECURRENT NOVAE: M31N 2008-12a AND THE IMPLICATIONS OF THE SWIFT NONDETECTION

A Self-consistent Model for a Full Cycle of Recurrent Novae—Wind Mass-loss Rate and X-Ray Luminosity

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

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