The nature and evolution of Nova Cygni 2006

Munari, U.; Siviero, A.; Henden, A. A.; Cardarelli, G.; Cherini, G.; Dallaporta, S.; Via, G. Dalla; Frigo, A.; Jurdana-Šepić, Rajka; Moretti, Stefano; Ochner, P.; Tomaselli, S.; Tomasoni, S.; Valisa, P.; Navasardyan, H.; Valentini, M.

doi:10.1051/0004-6361:200809502

Cited by 68 publications

(100 citation statements)

References 48 publications

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“…An increase of the observed colour index B−V from ∼0.1 to ∼0.55 between Aug. 15.0 and 19.2 (see Fig. 2 of Munari et al 2013a) corresponded to a change of the spectral type of the expanding envelope from ∼A2 to ∼F8 (cf. Cox 2000).…”

Section: Introductionmentioning

confidence: 94%

“…Relative flux units were converted into absolute fluxes with the aid of the (near-)simultaneous BVR C I C photometry of Munari et al (2013a) and/or UBV photometry from the AAVSO database. Magnitudes were converted to fluxes according to the calibration of Henden & Kaitchuck (1982).…”

Section: Observationsmentioning

confidence: 99%

“…First optical spectra were obtained on 2013 Aug. 14.844 by observers participating in the Astronomical Ring for Access to Spectroscopy (ARAS) project 1 (Shore et al 2013a) and by on 2013 Aug. 14.909. A&A 569, A112 (2014) A first description of the multicolour optical photometry was provided by Munari et al (2013a). They estimated the peak brightness of V339 Del to V ∼ 4.43, reached at Aug. 16.44 UT, that is, ∼1.85 days after its discovery.…”

Section: Introductionmentioning

confidence: 99%

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Early evolution of the extraordinary Nova Delphini 2013 (V339 Del)

Skopal

Drechsel

Тарасова

et al. 2014

A&A

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Aims. We determine the temporal evolution of the luminosity (L WD ), radius (R WD ) and effective temperature (T eff ) of the white dwarf (WD) pseudophotosphere of V339 Del from its discovery to around day 40. Another main objective was studying the ionization structure of the ejecta. Methods. These aims were achieved by modelling the optical/near-IR spectral energy distribution (SED) using low-resolution spectroscopy (3500-9200 Å), UBVR C I C and JHKLM photometry. Important insights in the physical conditions of the ejecta were gained from an analysis of the evolution of the Hα and Raman-scattered 6825 Å O vi line using medium-resolution spectroscopy (R ∼ 10 000). Results. During the fireball stage (Aug. 14. 8-19.9, 2013), T eff was in the range of 6000-12 000 K, R WD was expanding non-uniformly in time from ∼66 to ∼300 (d/3 kpc) R , and L WD was super-Eddington, but not constant. Its maximum of ∼9 × 10 38 (d/3 kpc) 2 erg s −1 occurred around Aug. 16.0, at the maximum of T eff , half a day before the visual maximum. After the fireball stage, a large emission measure of 1.0−2.0×10 62 (d/3 kpc) 2 cm −3 constrained the lower limit of L WD to be well above the super-Eddington value. The mass of the ionized region was a few ×10 −4 M , and the mass-loss rate was decreasing from ∼5.7 (Aug. 22) to ∼0.71× 10 −4 M yr −1 (Sept. 20).The evolution of the Hα line and mainly the transient emergence of the Raman-scattered O vi 1032 Å line suggested a biconical ionization structure of the ejecta with a disk-like H i region persisting around the WD until its total ionization, around day 40. On Sept. 20 (day 35), the model SED indicated a dust emission component in the spectrum. The dust was located beyond the H i zone, where it was shielded from the hard, > ∼ 10 5 K, radiation of the burning WD at that time. Conclusions. Our extensive spectroscopic observations of the classical nova V339 Del allowed us to map its evolution from the very early phase after its explosion. It is evident that the nova was not evolving according to the current theoretical prediction. The unusual non-spherically symmetric ejecta of nova V339 Del and its extreme physical conditions and evolution during and after the fireball stage represent interesting new challenges for the theoretical modelling of the nova phenomenon.

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Section: Introductionmentioning

confidence: 94%

Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Early evolution of the extraordinary Nova Delphini 2013 (V339 Del)

Skopal

Drechsel

Тарасова

et al. 2014

A&A

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“…Some novae (eg. Nova Aql 1994a, Nova Cyg 2006, Nova Cyg 2008bVenturini et al 2004, Munari et al 2008a, Munari et al 2011c, have displayed just one such event over their recorded photometric history. Strope et al (2010) in their review of AAVSO lightcurves of a hundred novae, termed J-type (from "jitter") the novae showing multiple secondary maxima.…”

Section: Photometric Evolutionmentioning

confidence: 99%

The hybrid, coronal lines nova V5588 Sgr (2011 N.2) and its six repeating secondary maxima

Munari¹,

Henden²,

Banerjee³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The outburst of Nova Sgr 2011 N.2 (=V5588 Sgr) was followed with optical and near-IR photometric and spectroscopic observations for 3.5 years, beginning shortly before the maximum. V5588 Sgr is located close to Galactic center, suffering from E B−V =1.56 (±0.1) extinction. The primary maximum was reached at V =12.37 on UT 2011 April 2.5 (±0.2), and the underlying smooth decline was moderately fast with t V 2 =38 and t V 3 =77 days. On top of an otherwise normal decline, six self-similar, fast evolving and bright secondary maxima (SdM) appeared in succession. Only very few other novae have presented so clear secondary maxima. Both the primary maximum and all SdM occurred at later times with increasing wavelengths, by amounts in agreement with expectations from fireball expansions. The radiative energy released during SdM declined following an exponential pattern, while the breadth of individual SdM and the time interval between them widened. Emission lines remained sharp (FWHM∼1000 km/s) throughout the whole nova evolution, with the exception of a broad pedestal with a trapezoidal shape (∆vel=3600 km/sec at the top and 4500 km/sec at the bottom) which was only seen during the advanced decline from SdM maxima and was absent in between SdM. V5588 Sgr at maximum light displayed a typical FeII-class spectrum which did not evolve into a nebular stage. About 10 days into the decline from primary maximum, a typical high-ionization He/N-class spectrum appeared and remained visible simultaneously with the FeII-class spectrum, qualifying V5588 Sgr as a rare hybrid nova. While the FeII-class spectrum faded into oblivion, the He/N-class spectrum developed strong [FeX] coronal lines.

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“…Pre-outburst optical photometry showed that it was varying by a few tenths of a magnitude, around ∼17.5 mag, up to about 10 d before eruption (Deacon et al 2014). Extensive broad-band optical photometry following the eruption was given by Munari et al (2013b). The visual light curve is given in Fig.…”

Section: 3 9 D E L P H I N Imentioning

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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The nature and evolution of Nova Cygni 2006

Cited by 68 publications

References 48 publications

Early evolution of the extraordinary Nova Delphini 2013 (V339 Del)

Early evolution of the extraordinary Nova Delphini 2013 (V339 Del)

The hybrid, coronal lines nova V5588 Sgr (2011 N.2) and its six repeating secondary maxima

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

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