A deep optical imaging study of the nebular remnants of classical novae

Slavin, Arthur J.; O’Brien, T. J.; Dunlop, James

doi:10.1093/mnras/276.2.353

Cited by 142 publications

(223 citation statements)

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“…From these modelled spectra it would seem that an ellipsoidal-like morphology may actually be more suited to the V1721 Aql ejecta, however we have far too little information to make a strong argument for this. We note that this higher axis ratio is contradictory to expectations in Slavin et al (1995). However, recent work on the 2010 outburst of U Sco by Drake & Orlando (2010) has indicated that nova ejecta can be significantly shaped by circumbinary gas and/or a high accretion disc gas density.…”

Section: The Nature Of the Secondarycontrasting

confidence: 90%

“…The blue and red peaks seen within the Hα and O I structures would therefore be the result of material ejected along the poles towards and away from the observer (observations and shaping models predict that the minor axis of a remnant lies in the disc plane; Slavin et al 1995;Porter et al 1998). This inclination however, would The nova systems presented here have not been corrected for extinction as in most cases the reddening is not accurately known, but it is assumed to be small to negligible in the near-IR for most Galactic novae systems.…”

Section: The Nature Of the Secondarymentioning

confidence: 99%

“…Given the speed of decline of the nova, work by Slavin et al (1995) would suggest that the axis ratio (ratio of semi-major to semi-minor axis) of Nova V1721 Aql's ejected shell is low (≈1). The nova ejecta may therefore be modelled by an approximately spherical shell with discreet randomly distributed knots of brighter emission.…”

Section: The Nature Of the Secondarymentioning

confidence: 99%

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A very luminous, highly extinguished, very fast nova – V1721 Aquilae

Hounsell

Darnley

Bode

et al. 2011

A&A

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Studies indicate that fast novae are primarily located within the plane of the Milky Way and slow novae are found within its bulge. Because of high interstellar extinction along the line of sight many novae lying close to the plane are missed and only the brightest seen. One nova lying very close to the Galactic plane is V1721 Aquilae, which was discovered in outburst on 2008 September 22.5 UT. Examination of spectra obtained 2.69 days after outburst revealed very high expansion velocities (FWHM of the Hα emission ≈6450 km s −1 ). In this paper we have used available pre-and post-outburst photometry and post-outburst spectroscopy to conclude that the object is a very fast, luminous, and highly extinguished (A V = 11.6 ± 0.2) nova system with an average ejection velocity of ≈3400 km s −1 . Pre-outburst near-IR colours from the 2MASS point source catalogue indicate that at quiescence the object is similar to many quiescent classical novae and appears to have a main sequence/sub-giant secondary rather than a giant counterpart. Based on the speed of decline of the nova and its emission line profiles we hypothesise that the axis ratio of the nova ejecta is ∼1.4 and that its inclination is such that the central binary accretion disc is face-on to the observer. As such, the accretion disc's blue contribution to the system's near-IR quiescent colours may be significant. Simple models of the nova ejecta have been constructed using the morphological modelling code XS5, and the results support the above hypothesis. Precise spectral classification of this object has been exceptionally difficult owing to low signal-to-noise levels and high extinction, which has eliminated all evidence of any He/N or Fe II emission within the spectra. We suggest two possibilities for the nature of V1721 Aql: that it is a U Sco type RN with a sub-giant secondary or, less likely, that it is a highly energetic bright and fast classical nova with a main sequence secondary. Future monitoring of the object for possible RN episodes may be worthwhile, as would archival searches for previous outbursts.

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Section: The Nature Of the Secondarycontrasting

confidence: 90%

Section: The Nature Of the Secondarymentioning

confidence: 99%

Section: The Nature Of the Secondarymentioning

confidence: 99%

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A very luminous, highly extinguished, very fast nova – V1721 Aquilae

Hounsell

Darnley

Bode

et al. 2011

A&A

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“…It is noteworthy that this expansion velocity is also comparable to the RN LMC 2009a (Bode et al, in prep. ) however, lower than those observed in other RNe (for example, RS Oph and U Sco, Ribeiro et al 2009;and Munari et al 1999, respectively) although still higher than a typical CN (e.g., Slavin et al 1995).…”

Section: Introductionmentioning

confidence: 53%

Historical light curve and search for previous outbursts of Nova KT Eridani (2009)

Jurdana-Šepić

Ribeiro

Darnley

et al. 2011

A&A

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Context. Nova Eridani (2009) caught the eye of the nova community due to its fast decline from maximum, which was initially missed, and its subsequent development in the radio and X-ray wavelengths. This system also exhibits properties similar to those of the much smaller class of recurrent novae; themselves potential progenitors of type Ia supernovae. Aims. We aim to determine the nature and physical parameters of the KT Eri progenitor system. Methods. We searched the Harvard College Observatory archive plates for the progenitor of KT Eri to determine the nature of the system, particularly the evolutionary stage of the secondary. We used the data obtained to search for any periodic signal and the derived luminosity to estimate a recurrence timescale. Furthermore, by comparing the colours of the quiescent system on a colour−magnitude diagram we may infer the nature of the secondary star. Results. We identified the progenitor system of KT Eri and measured a quiescent magnitude of B = 14.7 ± 0.4. No previous outburst was found. However, we suggest that if the nova is recurrent it should be on a timescale of centuries. We find a periodicity at quiescence of 737 days which may arise from reflection effects and/or eclipses in the central binary. The periodicity and the quiescence magnitude of the system suggest that the secondary star is evolved and likely in, or ascending, the Red Giant Branch. A second period is evident at 376 days which has a sinusoidal like light curve. Furthermore, the outburst amplitude of ∼9 mag is inconsistent with those expected for fast classical novae (∼17 mag) which may lend further support for an evolved secondary. Conclusions. We investigated the probable recurrent nova KT Eri for which we suggest an inter-outburst period of order centuries and an evolved secondary. This may suggest that there is a whole range of possible inter-outburst periods in between the "typical" classical and recurrent novae nomenclature. Archival searches are an excellent tool in order to investigate the nature of astrophysical objects, in order to determine the nature and physical parameters.

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“…These derived lower limits should be smaller than the actual n e values because τ (Br γ ) can be considerably >1. An additional caveat in this analysis is the intrinsic assumption of spherical geometry for the ejecta (Slavin, O'Brien & Dunlop 1995), since a bipolar morphology appears more appropriate for V339 Del (see also Schaefer et al 2014;Shore et al 2016).…”

Section: Case B Analysismentioning

confidence: 99%

Rise and fall of the dust shell of the classical nova V339 Delphini

Evans

Banerjee

Gehrz³

et al. 2017

Mon. Not. R. Astron. Soc.

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We present infrared spectroscopy of the classical nova V339 Del, obtained over an ∼2-yr period. The infrared emission lines were initially symmetrical, with half width half-maximum velocities of 525 km s −1 . In later (t 77 d, where t is the time from outburst) spectra, however, the lines displayed a distinct asymmetry, with a much stronger blue wing, possibly due to obscuration of the receding component by dust. Dust formation commenced at approximately day 34.75 at a condensation temperature of 1480 ± 20 K, consistent with graphitic carbon. Thereafter, the dust temperature declined with time as T d ∝ t −0.346 , also consistent with graphitic carbon. The mass of dust initially rose, as a result of an increase in grain size and/or number, peaked at approximately day 100, and then declined precipitously. This decline was most likely caused by grain shattering due to electrostatic stress after the dust was exposed to X-radiation. The appendix summarizes Planck means for carbon and the determination of grain mass and radius for a carbon dust shell.

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A deep optical imaging study of the nebular remnants of classical novae

Cited by 142 publications

References 0 publications

A very luminous, highly extinguished, very fast nova – V1721 Aquilae

A very luminous, highly extinguished, very fast nova – V1721 Aquilae

Historical light curve and search for previous outbursts of Nova KT Eridani (2009)

Rise and fall of the dust shell of the classical nova V339 Delphini

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