Breaking the Habit: The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a

Henze, M.; Darnley, M. J.; Williams, S. C.; Kato, Mariko; Hachisu, Izumi; Anupama, G. C.; Arai, Akira; Boyd, David; Burke, Douglas; Ciardullo, Robin; Chinetti, K.; Cook, Lewis M.; Cook, Michael J.; Erdman, P. W.; Gao, Xing; Harris, B.; Hartmann, D. H.; Hornoch, K.; Horst, J. Chuck; Hounsell, R.; Husar, D.; Itagaki, K.; Kabashima, F.; Kafka, S.; Kaur, A.; Kiyota, S.; Kojiguchi, Naoto; Kučáková, H.; Kuramoto, Kiyoshi; Maehara, Hiroyuki; Mantero, A.; Masci, Frank J.; Matsumoto, Katsura; Naito, H.; Ness, J. U.; Nishiyama, K.; Oksanen, A.; Osborne, J. P.; Page, K. L.; Paunzen, E.; Pavana, M.; Pickard, R.; Prieto-Arranz, J.; Rodríguez‐Gil, P.; Sala, G.; Sano, Y.; Shafter, A. W.; Sugiura, Yuki; Tan, Hanjie; Tordai, Tamás; Vraštil, J.; Wagner, R. M.; Watanabe, F.; Williams, Benjamin F.; Bode, M. F.; Bruno, A.; Buchheim, B.; Crawford, Tim; Goff, B.; Hernanz, M.; Igarashi, A. S.; José, J.; Motta, Mário; O’Brien, T. J.; Oswalt, Terry D.; Poyner, G.; Ribeiro, V. A. R. M.; Sabo, Richard; Shara, Michael M.; Shears, Jeremy; Starkey, Donn R.; Starrfield, S.; Woodward, C. E.

doi:10.3847/1538-4357/aab6a6

Cited by 33 publications

(47 citation statements)

References 89 publications

(116 reference statements)

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“…Morii et al (2016) placed limits on X-ray flashes for 40 novae using the Monitor of All-sky X-ray Image (MAXI; Matsuoka et al, 2009); however, the energy band of the Gas Slit Camera at 2-4 keV is likely too high to detect the expected SSS emission. The most rapidly recurrent nova known to date, M31N 2008-12a (Henze et al, 2018, and references therein), has a recurrence timescale of close to 1 yr, making it a suitable candidate for monitoring for precursive flashes. A high cadence (approximately every 6 hr) monitoring campaign was carried out by Swift during the 8-day run-up to the eventual 2015 outburst (Kato et al, 2016).…”

Section: Open Questionsmentioning

confidence: 99%

Neil Gehrels Swift Observatory studies of supersoft novae

Page

Beardmore

Osborne

2020

Advances in Space Research

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The rapid response capabilities of the Neil Gehrels Swift Observatory, together with the daily planning of its observing schedule, make it an ideal mission for following novae in the X-ray and UV bands, particularly during their early phases of rapid evolution and throughout the supersoft source interval. Many novae, both classical and recurrent, have been extensively monitored by Swift throughout their supersoft phase and later decline. We collect here results from observations of novae with outbursts which occurred between the start of 2006 and the end of 2017.

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Section: Open Questionsmentioning

confidence: 99%

Neil Gehrels Swift Observatory studies of supersoft novae

Page

Beardmore

Osborne

2020

Advances in Space Research

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“…However, it does not provide strong evidence in isolation. Additionally, the spectrum obtained during the plateau shows no evidence for narrow (or any) He ii lines, a key signature of a hot disk (as in seen during the plateau phase of known recurrent novae; e.g., Henze et al 2018).…”

Section: A Possibly 'Faint and Fast' Or Recurrent Nova?mentioning

confidence: 91%

AT 2017fvz: a nova in the dwarf irregular galaxy NGC 6822

Healy

Darnley

Copperwheat

et al. 2019

Monthly Notices of the Royal Astronomical Society

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A transient in the Local Group dwarf irregular galaxy NGC 6822 (Barnard's Galaxy) was discovered on 2017 August 2 and is only the second classical nova discovered in that galaxy. We conducted optical, near-ultraviolet, and X-ray follow-up observations of the eruption, the results of which we present here. This 'very fast' nova had a peak V-band magnitude in the range −7.41 > M V > −8.33 mag, with decline times of t 2,V = 8.1 ± 0.2 d and t 3,V = 15.2 ± 0.3 d. The early-and late-time spectra are consistent with an Fe ii spectral class. The Hα emission line initially has a full width at halfmaximum intensity of ∼ 2400 km s −1 -a moderately fast ejecta velocity for the class. The Hα line then narrows monotonically to ∼ 1800 km s −1 by 70 d post-eruption. The lack of a pre-eruption coincident source in archival Hubble Space Telescope imaging implies that the donor is a main sequence, or possibly subgiant, star. The relatively low peak luminosity and rapid decline hint that AT 2017fvz may be a 'faint and fast' nova.

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“…Therefore, Maccarone et al (2019) expected the orbital period of ASASSN-16oh to be several days. Maccarone et al (2019) concluded that ASASSN-16oh is not a classical nova (thermonuclear runaway event) but an accretion event like a dwarf nova, mainly because (1) the optical spectra show a very narrow width of He II emission with no signature of mass-ejection, (2) very slow rise (∼ 200 days) to the optical maximum compared with those of classical novae (a few days), (3) rather dark peak V magnitude of M V,max ∼ −2.3 compared with those of recurrent novae (e.g., the 1 year recurrence period nova M31N 2008-12a of M V,max = −7.2, Darnley et al 2015;Henze et al 2018).…”

Section: Introductionmentioning

confidence: 99%

ASASSN-16oh: A Nova Outburst with No Mass Ejection—A New Type of Supersoft X-Ray Source in Old Populations

Kato

Saio

Hachisu

2020

ApJ

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ASASSN-16oh is a peculiar transient supersoft X-ray source without a mass ejection signature in the field of the Small Magellanic Cloud. Maccarone et al. (2019) concluded that ASASSN-16oh is the first dwarf nova with supersoft X-ray that originated from an equatorial accretion belt on a white dwarf (WD). Hillman et al. (2019) proposed a thermonuclear runaway model that both the X-rays and V /I photons are emitted from the hot WD. We calculated the same parameter models as Hillman et al.'s and found that they manipulated on/off the mass-accretion, and their best fit V light curves are 6 mag fainter, and decay about 10 times slower, than that of ASASSN-16oh. We propose a nova model induced by a high rate of mass-accretion during a dwarf nova outburst, i.e., the X-rays originate from the surface of the hydrogen-burning WD whereas the V /I photons are from the irradiated disk. Our model explains the main observational properties of ASASSN-16oh. We also obtained thermonuclear runaway models with no mass ejection for a wide range of parameters of the WD mass and massaccretion rates including both natural and forced novae in low-metal environments of Z = 0.001 and Z = 0.0001. They are a new type of periodic supersoft X-ray sources with no mass ejection, and also a bright transient in V /I bands if they have a large disk. We suggest that such objects are candidates of Type Ia supernova progenitors because its mass is increasing at a very high efficiency (∼ 100%).

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Breaking the Habit: The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a

Abstract: Since its discovery in 2008, the Andromeda galaxy nova M31N 2008-12a has been observed in eruption every single year. This unprecedented frequency indicates an extreme object, with a massive white dwarf and a high accretion rate,

Cited by 33 publications

References 89 publications

Neil Gehrels Swift Observatory studies of supersoft novae

Neil Gehrels Swift Observatory studies of supersoft novae

AT 2017fvz: a nova in the dwarf irregular galaxy NGC 6822

ASASSN-16oh: A Nova Outburst with No Mass Ejection—A New Type of Supersoft X-Ray Source in Old Populations

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