<i>BVI</i> photometry and the spectroscopy of Nova Scuti 2005 N.2

Munari, U.; Siviero, A.; Navasardyan, H.; Dallaporta, S.

doi:10.1051/0004-6361:20054720

Cited by 20 publications

(18 citation statements)

References 9 publications

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“…The bump event itself, far from being near the optically-thin regime, cannot be modeled without comprehensive radiative transfer calculations. Assuming an instrument resolution folding of 0.6 nm, the narrow emission profile perfectly fits that of two independent optically-thin expanding shells modeled after Lamers & Cassinelli (1999), at the velocities reported by Siviero et al (2006) and Munari et al (2006b). The thickness of the shells are assumed to be negligible compared to their radii at this time.…”

Section: The Evolution Of the H α Linesupporting

confidence: 63%

The unusual Nova Cygni 2006 (V2362 Cygni)

Kimeswenger¹,

Dalnodar²,

Knapp³

et al. 2008

A&A

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Context. Optical nova lightcurves often have structures, such as rapid declines and recoveries, due to nebular or dusty phases of the ejecta. Nova Cygni 2006 (V2362 Cyg) underwent an unusual brightening after an early rapid decline. The shape of the lightcurve can be compared to that of V1493 Aql, but in that case the whole event was not as bright and only lasted a couple of weeks. V2362 Cyg had a moderately fast decline of t 2 = 9.0 ± 0.5 days before rebrightening, which lasted 250 days after maximum. Aims. We present an analysis of our own spectroscopic investigations in combination with American Association of Variable Star Observers (AAVSO) photometric data covering the whole rebrightening phase until the return to the final decline. Methods. We used medium resolution spectroscopy obtained in ten observing nights in the course of 79 nights to investigate the change of the velocity structure of the ejecta. The publicly available AAVSO photometry was used to analyze the overall properties and the energy of the brightening. Results. Although the behavior of the main outburst (velocity, outburst magnitude, and decline timescales) resembles a "normal" classical nova, the shell clearly underwent a second fast mass ejecting phase, causing the unusual properties. The integrated flux during this event contributes ≈40% to the total radiation energy of the outburst. The evolution of the H α profile during the bump event is obtained by subtracting the emission of the detached shells of the main eruption by a simple optically-thin model. A distance of D ≈ 7.5 +3.0 −2.5 kpc and an interstellar extinction E(B − V) = 0. m 6 ± 0. m 1 was also derived.

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Section: The Evolution Of the H α Linesupporting

confidence: 63%

The unusual Nova Cygni 2006 (V2362 Cygni)

Kimeswenger¹,

Dalnodar²,

Knapp³

et al. 2008

A&A

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“…While V2672 Oph is undoubtedly away from the bulge, its height above the Galactic plane is difficult to reconcile with the z ≤ 100 –200 pc found by della Valle & Livio (1998) for He/N novae. The proportion of He/N novae characterized by high z is becoming uncomfortably large in comparison with the della Valle & Livio (1998) scaleheight – other recent high‐ z examples being V2491 Cyg (= Nova Cyg 2008 N.2) at z = 1.1 kpc (Munari et al 2010b) and V477 Sct (= Nova Sct 2005 N2), located at z = 0.6 kpc (Munari et al 2006).…”

Section: Photometric Evolutionmentioning

confidence: 99%

Properties, evolution and morpho-kinematical modelling of the very fast nova V2672 Oph (Nova Oph 2009), a clone of U Sco

Munari

Ribeiro

Bode

et al. 2010

Monthly Notices of the Royal Astronomical Society

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Nova Oph 2009 (V2672 Oph) reached maximum brightness V= 11.35 on 2009 August 16.5. With observed t2(V) = 2.3 and t3(V) = 4.2 d decline times, it is one of the fastest known novae, being rivalled only by V1500 Cyg (1975) and V838 Her (1991) among classical novae, and U Sco among the recurrent ones. The line of sight to the nova passes within a few degrees of the Galactic Centre. The reddening of V2672 Oph is E(B−V) = 1.6 ± 0.1, and its distance d∼ 19 kpc places it on the other side of the Galactic Centre at a galactocentric distance larger than the solar one. The lack of an infrared counterpart for the progenitor excludes the donor star from being a cool giant like in RS Oph or T CrB. With close similarity to U Sco, V2672 Oph displayed a photometric plateau phase, a He/N spectrum classification, extreme expansion velocities and triple peaked emission‐line profiles during advanced decline. The full width at zero intensity of Hα was 12 000 km s−1 at maximum, and declined linearly in time with a slope very similar to that observed in U Sco. The properties displayed by V2672 Oph lead us to infer a mass of its white dwarf close to the Chandrasekhar limit and a possible final fate as a Type Ia supernova. Morpho‐kinematical modelling of the evolution of the Hα profile suggests that the overall structure of the ejecta is that of a prolate system with polar blobs and an equatorial ring. The density in the prolate system appeared to decline faster than that in the other components. V2672 Oph is seen pole‐on, with an inclination of 0°± 6° and an expansion velocity of the polar blobs of 4800+900−800 km s−1. On the basis of its remarkable similarity to U Sco, we suspect this nova may be a recurrent. Given the southern declination, the faintness at maximum, the extremely rapid decline and its close proximity to the ecliptic, it is quite possible that previous outbursts of V2672 Oph have been missed.

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“…As a He/N nova, NCyg08-2 is unusually high above the galactic plane, it laying at z=1.1 kpc, much larger than the scale height of ≤100 pc estimated by della Valle and Livio (1998) for He/N novae. Other He/N novae high above the Galactic plane were V477 Sct (= Nova Sct 2005 N2), located at z=0.6 kpc (Munari et al, 2006), or V2672 Oph (= Nova Oph 2009) at z=0.8 kpc (Munari et al 2010c).…”

Section: Spectral Evolutionmentioning

confidence: 99%

An extensive optical study of V2491 Cyg (Nova Cyg 2008 N.2), from maximum brightness to return to quiescence

Munari

Siviero

Dallaporta³

et al. 2011

New Astronomy

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The photometric and spectroscopic evolution of the He/N and very fast Nova Cyg 2008 N2 (V2491 Cyg) is studied in detail. A primary maximum was reached at V=7.45±0.05 on April 11.37 (±0.1) 2008 UT, followed by a smooth decline characterized by t V 2 =4.8 days, and then a second maximum was attained at V=9.49±0.03, 14.5 days after the primary one. This is the only third nova to have displayed a secondary maximum, after V2362 Cyg and V1493 Aql. The development and energetics of the secondary maximum is studied in detail. The smooth decline that followed was accurately monitored until day +144 when the nova was 8.6 mag fainter than maximum brightness, well into its nebular phase, with its line and continuum emissivity declining as t −3 . The reddening affecting the nova was E B−V =0.23±0.01, and the distance of 14 kpc places the nova at a height above the galactic plane of 1.1 kpc, larger than typical for He/N novae. The expansion velocity of the bulk of ejecta was 2000 km/sec, with complex emission profiles and weak P-Cyg absorptions during the optically thick phase, and saddle-like profiles during the nebular phase. Photo-ionization analysis of the emission line spectrum indicates that the mass ejected by the outburst was 5.3 10 −6 M ⊙ and the mass fractions to be X=0.573, Y=0.287, Z=0.140, with those of individual elements being N=0.074, O=0.049, Ne=0.015. The metallicity of the accreted material was [Fe/H]=−0.25, in line with ambient value at the nova galacto-centric distance. Additional spectroscopic and photometric observations at days +477 and +831 show the nova returned to the brightness level of the progenitor and to have resumed the accretion onto the white dwarf.

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BVI photometry and the spectroscopy of Nova Scuti 2005 N.2

Cited by 20 publications

References 9 publications

The unusual Nova Cygni 2006 (V2362 Cygni)

The unusual Nova Cygni 2006 (V2362 Cygni)

Properties, evolution and morpho-kinematical modelling of the very fast nova V2672 Oph (Nova Oph 2009), a clone of U Sco

An extensive optical study of V2491 Cyg (Nova Cyg 2008 N.2), from maximum brightness to return to quiescence

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