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

Kato, Mariko; Saio, Hideyuki; Hachisu, Izumi

doi:10.3847/1538-4357/838/2/153

Cited by 28 publications

(62 citation statements)

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“…In particular, the interpretation of the UV observations in this work, the UV and X-ray observations reported by Henze et al (2014), DHS15, HND15, and DHB16, and the theoretical work by Kato et al (2014Kato et al ( , 2015Kato et al ( , 2016Kato et al ( , 2017, are especially sensitive to the adopted value of the extinction.…”

Section: Extinctionmentioning

confidence: 81%

No Neon, but Jets in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Spectroscopy of the 2015 Eruption

Darnley

Hounsell

Godon

et al. 2017

ApJ

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The 2008 discovery of an eruption of M31N 2008-12a began a journey on which the true nature of this remarkable recurrent nova continues to be revealed. M31N 2008-12a contains a white dwarf (WD) close to the Chandrasekhar limit, accreting at a high rate from its companion, and undergoes thermonuclear eruptions that are observed yearly and may even be twice as frequent. In this paper, we report on Hubble Space Telescope Space Telescope Imaging Spectrograph ultraviolet spectroscopy taken within days of the predicted 2015 eruption, coupled with Keck spectroscopy of the 2013 eruption. Together, this spectroscopy permits the reddening to be constrained to0.10 0.03. The UV spectroscopy reveals evidence for highly ionized, structured, and highvelocity ejecta at early times. No evidence for neon is seen in these spectra, however, but it may be that little insight can be gained regarding the composition of the WD (CO versus ONe).

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Section: Extinctionmentioning

confidence: 81%

No Neon, but Jets in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Spectroscopy of the 2015 Eruption

Darnley

Hounsell

Godon

et al. 2017

ApJ

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“…As in Figure 4, comparing the best-fit accretion disk models to the HST photometry ∼75 days post-eruption-the minimum state. Also shown, in magenta and cyan, are our predicted accretion disk spectra based on an accretion rate of =´-- M M 1.6 10 yr 7 1 , as required by Kato et al (2014Kato et al ( , 2015Kato et al ( , 2016Kato et al ( , 2017b. Disks with the Kato et al accretion rate underpredict the quiescent flux of M31N 2008-12a by a factor of ∼10.…”

Section: The Accretion Diskmentioning

confidence: 91%

“…The models, discussed below, generate the disk mass accretion rate (Ṁ), whereas the existing M31N 2008-12a eruption models of Kato et al (2014Kato et al ( , 2015Kato et al ( , 2016Kato et al ( , 2017aKato et al ( , 2017b are concerned with the WD mass accretion rate (Ṁ acc ), the amount of material that falls onto the WD surface itself.…”

Section: Modeling the Accretion Diskmentioning

confidence: 99%

“…But we note, of course, that the former (with no upper limit) poses no clear obstacle to our derived accretion rates. Turning to the latter, we note that the work of Kato et al (2014Kato et al ( , 2015Kato et al ( , 2016Kato et al ( , 2017aKato et al ( , 2017b, employing such a formulation, has already successfully modeled many observational aspects of the M31N 2008-12a eruptions, while assuming a constant =´-…”

Section: The Accretion Diskmentioning

confidence: 99%

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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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“…The small zig-zag path between logT (K) ∼ 5.5 and 5.0 is due to the change in chemical composition, i.e., the surface layer with the original composition of accreted matter is blown away in the wind. The data are taken from [58].…”

Section: Physics Of Super-eddington Luminositymentioning

confidence: 99%

Multifrequency behavior of classical novae

Hachisu

Kato²

2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

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We review our current understanding of multiwavelength light curves of classical and recurrent novae and show how to determine the WD masses and other binary properties. We pick up PW Vul, U Sco, V745 Sco, RS Oph, and V407 Cyg as representatives of different types of light curves, examine their light curves in detail, discuss physical properties, and clarify the reason of these differences. In the rising phase, the hydrogen-rich envelope expands beyond the size of a close binary in which the companion is embedded deep inside of the photosphere. After the optical maximum, the pseud-photosphere begins to shrink and an optically thin region develops outside of the photosphere. The free-free emission dominates the flux at relatively longer wavelengths (optical and NIR), of which light curves decay along the universal decline law of F ν ∝ t −1.75 (or t −1.55). The physical mechanism of super-Eddington phase is presented. In the presence of shock interaction between ejecta and circumstellar matter, it slows down the decay of optical flux as F ν ∝ t −1.0 as seen in the early phase of V407 Cyg. In final stages of outbursts, the wind mass-loss rate sharply drops so the slope of free-free emission decays like F ν ∝ t −3.5. Supersoft X-ray phase begins and continues until hydrogen nuclear burning ends, and after that the nova enters a cooling phase. Hard X-rays may originate from internal shocks between ejecta (or a bow shock between ejecta and the companion). The behaviors of optical-dominant, UV-dominant, and supersoft X-ray source phase have different dependences on the WD mass and envelope chemical composition, so multiwavelength observations are useful to determine the parameters such as the WD mass. Finally, we should note that the very early phase of nova outbursts remains unexplored. An X-ray flash phase is theoretically identified, but not yet successfully detected. Detections of early X-ray flashes give direct information on thermonuclear runaway.

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

Cited by 28 publications

References 50 publications

No Neon, but Jets in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Spectroscopy of the 2015 Eruption

No Neon, but Jets in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Spectroscopy 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

Multifrequency behavior of classical novae

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