The 2010 nova outburst of the symbiotic Mira V407 Cyg

Munari, U.; Joshi, Vishal; Ashok, N. M.; Banerjee, D. P. K.; Valisa, P.; Milani, Andrea; Siviero, A.; Dallaporta, S.; Castellani, F.

doi:10.1111/j.1745-3933.2010.00979.x

Cited by 78 publications

(120 citation statements)

References 20 publications

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“…A major difference with RS Oph (Skopal et al 2008) and V407 Cyg (Munari et al 2011), is the lack of an even sharper absorption superimposed to the narrow component. This very sharp absorption (FWHM∼15 km sec −1 ) originates is the outer neutral portion of the wind not reached by the initial UV-flash, which is completely absorbed by the gas inner to it.…”

Section: The Narrow Componentmentioning

confidence: 99%

“…There is however a very rare type of nova (∼3% of the total, Williams et al 2014) in which the initial UV flash interacts with dense pre-existing circumstellar material, the prototypes being the recurrent novae RS Oph and V407 Cyg Munari et al 2011). In such systems, the WD orbits -with periods of a few years -within the extended wind of a late type giant companion.…”

Section: Introductionmentioning

confidence: 99%

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Flash-ionization of pre-existing circumstellar material around Nova Oph 2015

Munari

Walter

2015

Monthly Notices of the Royal Astronomical Society: Letters

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We have obtained daily high resolution Echelle spectroscopy of Nova Oph 2015 during its initial evolution. It reveals the presence of pre-existing circumstellar material around the nova, which is best interpreted as the wind of an evolved companion. On earliest observations, the emission line profiles of Nova Oph 2015 displayed a very narrow emission component (FWHM∼60 km sec −1 ), recombining over a time scale of 5 days and showing constant low velocity (RV ⊙ =−4.5 km sec −1 ), that we interpret as coming from the wind of the secondary recombining after the ionization from the initial UV-flash of the nova. The underlying broad component underwent a marked reduction in both FWHM and width at zero intensity (the latter declining from 4000 to 2000 km sec −1 in ten days) while increasing by 6× in flux, that we believe is the result of the high velocity ejecta of the nova being slowed down while trying to expand within the surrounding wind of the companion. Novae with evolved secondaries are very rare in the Galaxy, amounting to ∼3% of the total according to recent estimates. Among them Nova Oph 2015 is perhaps unique in having displayed a long rise to maximum brightness and a slow decline from it, a FeII-type classification (contrary to prevailing He/N) and a probable sub-giant luminosity class for the secondary (instead of the giant (e.g. RS Oph) or supergiant (e.g. V407 Cyg) class for the others).

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Section: The Narrow Componentmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Flash-ionization of pre-existing circumstellar material around Nova Oph 2015

Munari

Walter

2015

Monthly Notices of the Royal Astronomical Society: Letters

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“…Adding to this, observations of PMS stars are usually made difficult by their faintness in quiescence and by the disturbance from sometimes heavy dust extinction, either surrounding the star or diffuse through the star forming region. Therefore, the rare outbursts of PMS stars always attract considerable interest, especially when they are long lasting, as in the case of new FUor objects (from the name of the prototype of this class, FU Ori), with one of the most recent and spectacular cases being that of HBC 722 = V2493 Cyg (Semkov et al 2010;Miller et al 2011;Munari et al 2010;Leoni et al 2010;Kóspál et al 2011;Armond et al 2011;Green et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Long-term photometric observations of pre-main sequence objects in the field of North America/Pelican Nebula

Beljan

Jurdana-Šepić

Semkov

et al. 2014

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To broaden the search and study stars in the early evolutionary phase, we investigated a sample of 17 pre-main sequence objects previously detected as either Hα emission-line pre-main sequence stars or T Tauri variables located in the field of the North America/Pelican Nebula complex. Johnson-Cousins B, V, R c , I c magnitudes and mean color indices for the program stars are determined from more than 12 400 measurements from archive photographic plates and from CCD data collected at 7 observatories covering the period of almost 60 years from 1954 up to 2013. We complemented previously rare insights on the photometry of the program stars and presented their photometric history, which for almost all program stars is the first long term photometric monitoring on a timescale of 6 decades. Eight program stars are found to be classical T Tauri stars of variability type II, while 6 program stars are weak-line T Tauri stars of variability type I. For the first time, periodicity is found for three stars: V1716 Cyg indicates a 4.15 day period, V2051 Cyg indicates a 384 day period, and V521 Cyg a period of 503 days.

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“…While these latter lines grow in prominence, their FWHM however rapidly declines as a consequence of the ejecta being slowed down while trying to expand through the surrounding medium. As an example, during the 2010 outburst of the NwSS V407 Cyg, Munari et al (2011a) measured e-folding times of 4 days for the recombination of the flash-ionized gas and of 3 days for the deceleration of the ejecta.…”

Section: Introductionmentioning

confidence: 99%

“…Evans et al 2008, Das et al 2006 and V407 Cyg in 2010 (e.g. Munari et al 2011a) are template cases. The powerful initial UV-flash accompanying the TNR onset goes undetected by observers and is lost into surrounding emptiness in the case of classical novae whereas in the NwSS it ionizes the circumstellar gas originating from the wind of the giant.…”

Section: Introductionmentioning

confidence: 99%

Infrared spectroscopy of the remnant of Nova Sco 2014: a symbiotic star with too little circumstellar matter to decelerate the ejecta

Munari

Banerjee

2017

Monthly Notices of the Royal Astronomical Society

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Pre-outburst 2MASS and WISE photometry of Nova Sco 2014 (V1534 Sco) have suggested the presence of a cool giant at the location of the nova in the sky. The spectral evolution recorded for the nova did not however support a direct partnership because no flash-ionized wind and no deceleration of the ejecta were observed, contrary to the behavior displayed by other novae which erupted within symbiotic binaries like V407 Cyg or RS Oph. We have therefore obtained an 0.8−2.5 µm spectra of the remnant of Nova Sco 2014 in order to ascertain if a cool giant is indeed present and if it is physically associated with the nova. The spectrum shows the presence of a M6III giant, reddened by E(B-V)=1.20, displaying the typical and narrow emission-line spectrum of a symbiotic star, including HeI 1.0830 µm with a deep P-Cyg profile. This makes Nova Sco 2014 a new member of the exclusive club of novae that erupt within a symbiotic binary. Nova Sco 2014 shows that a nova erupting witin a symbiotic binary does not always come with a deceleration of the ejecta, contrary to the common belief. Many other similar systems may lay hidden in past novae, expecially in those that erupted prior to the release of the 2MASS all-sky infrared survey, which could be profitably cross-matched now against them.

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The 2010 nova outburst of the symbiotic Mira V407 Cyg

Cited by 78 publications

References 20 publications

Flash-ionization of pre-existing circumstellar material around Nova Oph 2015

Flash-ionization of pre-existing circumstellar material around Nova Oph 2015

Long-term photometric observations of pre-main sequence objects in the field of North America/Pelican Nebula

Infrared spectroscopy of the remnant of Nova Sco 2014: a symbiotic star with too little circumstellar matter to decelerate the ejecta

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