On the Progenitors of Galactic Novae

Darnley, M. J.; Ribeiro, V. A. R. M.; Bode, M. F.; Hounsell, R.; Williams, R.

doi:10.1088/0004-637x/746/1/61

Cited by 90 publications

(139 citation statements)

References 50 publications

(38 reference statements)

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“…Mróz et al (2015) determined an orbital period of P = 1.59230(5) days using data from the OGLE survey, and suggest that the system likely contains a subgiant secondary and a massive white dwarf. This is a relatively unusual part of nova-progenitor parameter space, with only a few such systems known (Darnley et al 2012). Mróz et al (2015) additionally observed eclipses in the quiescent optical light curve, indicating that the inclination is close to 90 • (Mróz et al 2015).…”

Section: Introductionmentioning

confidence: 89%

Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)

Weston

Sokoloski

Chomiuk

et al. 2016

Mon. Not. R. Astron. Soc.

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Since the Fermi discovery of γ-rays from novae, one of the biggest questions in the field has been how novae generate such high-energy emission. Shocks must be a fundamental ingredient. Six months of radio observations of the 2012 nova V5589 Sgr with the VLA and 15 weeks of X-ray observations with Swift/XRT show that the radio emission consisted of: 1) a shock-powered, non-thermal flare; and 2) weak thermal emission from 10 −5 M of freely expanding, photoionized ejecta. Absorption features in the optical spectrum and the peak optical brightness suggest that V5589 Sgr lies 4 kpc away (3.2-4.6 kpc). The shock-powered flare dominated the radio light curve at low frequencies before day 100. The spectral evolution of the radio flare, its high radio brightness temperature, the presence of unusually hard (kT x > 33 keV) X-rays, and the ratio of radio to X-ray flux near radio maximum all support the conclusions that the flare was shock-powered and non-thermal. Unlike most other novae with strong shock-powered radio emission, V5589 Sgr is not embedded in the wind of a redgiant companion. Based on the similar inclinations and optical line profiles of V5589 Sgr and V959 Mon, we propose that shocks in V5589 Sgr formed from collisions between a slow flow with an equatorial density enhancement and a subsequent faster flow. We speculate that the relatively high speed and low mass of the ejecta led to the unusual radio emission from V5589 Sgr, and perhaps also to the non-detection of γ-rays.

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Section: Introductionmentioning

confidence: 89%

Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)

Weston

Sokoloski

Chomiuk

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The shorter recurrence periods are driven by a combination of a high-mass WD and a high mass accretion rate. Such high accretion rates are typically driven by an evolved companion star, such as a Roche lobe overflowing sub-giant star (SG-novae; also the U Scorpii type of RNe) or the stellar wind from a red giant companion (RG-novae: symbiotic novae, or the RS Ophiuchi type RNe; see Darnley et al 2012Darnley et al , 2014a, for recent reviews).…”

Section: Introductionmentioning

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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“…In addition to the class of persistent SSS, classical novae (CNe) have frequently been observed to emit an SSS spectrum during the later phase of their outburst. It is now commonly accepted that SSS emission originates in binary systems containing a white dwarf primary that hosts nuclear burning of material that is accreted from a secondary star; see van den Heuvel et al (1992) and Kahabka & van den Heuvel (1997), as well as Darnley et al (2012) for discussion of types and the role of the secondary star in nova systems. In persistent SSS, the burning rate is roughly the same as the accretion rate (van den Heuvel et al 1992;Kahabka & van den Heuvel 1997), while in novae during outburst, the burning rate is higher, eventually leading the SSS emission to disappear once all hydrogen is consumed.…”

Section: Introductionmentioning

confidence: 99%

Obscuration effects in super-soft-source X-ray spectra

Ness

Osborne

Henze

et al. 2013

A&A

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Context. Super-soft-source (SSS) X-ray spectra are blackbody-like spectra with effective temperatures ∼3−7 × 10 5 K and luminosities of 10 35−38 erg s −1 . Grating spectra of SSS and novae in outburst that show SSS type spectra display atmospheric absorption lines. Radiation transport atmosphere models can be used to derive physical parameters. Blue-shifted absorption lines suggest that hydrostatic equilibrium is an insufficient assumption, and more sophisticated models are required. Aims. In this paper, we bypass the complications of spectral models and concentrate on the data in a comparative, qualitative study. We inspect all available X-ray grating SSS spectra to determine systematic, model-independent trends. Methods. We collected all grating spectra of conventional SSS like Cal 83 and Cal 87 plus observations of novae during their SSS phase. We used comparative plots of spectra of different systems to find common and different features. The results were interpreted in the context of system parameters obtained from the literature.

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On the Progenitors of Galactic Novae

Cited by 90 publications

References 50 publications

Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)

Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)

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

Obscuration effects in super-soft-source X-ray spectra

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