A Near-Infrared Shock Wave in the 2006 Outburst of Recurrent Nova RS Ophiuchi

Das, Ramkrishna; Banerjee, D. P. K.; Ashok, N. M.

doi:10.1086/510674

Cited by 54 publications

(87 citation statements)

References 11 publications

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“…Using this method, we find an ejected mass of 3.4 × 10 −6 M ⊙ and 4.9 × 10 −6 M ⊙ for D31 and D49, respectively. Similar values of 1 -3 × 10 −6 M ⊙ and 3 × 10 −6 M ⊙ were estimated from other studies (e.g., Das et al 2006;Kato, Hachisu & Luna 2008) …”

Section: Estimation Of the Ejecta Masssupporting

confidence: 89%

“…The nova light curves also behave similarly; they decline fast with t 2 ∼ 6 and t 3 ∼ 17 days (Rosino 1987, Munari et al 2007). The key result of the 1985 and 2006 observations was the detection of a shock that is generated while the ejecta interacts with the surrounding wind of the red giant secondary (Bode & Kahn 1985, Das et al 2006 and references therein) and a non-spherical bi-polar shape of the nova ejecta (e.g., Taylor et al 1989, Chesneau et al 2007, Bode et al 2007). Further investigations also helped to determine a few important parameters viz.…”

Section: Introductionmentioning

confidence: 99%

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Abundance analysis of the recurrent nova RS Ophiuchi (2006 outburst)

Das

Mondal

2015

New Astronomy

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We present an analysis of elemental abundances of ejecta of the recurrent nova RS Oph using published optical and near-infrared spectra during the 2006 outburst. We use the CLOUDY photoionization code to generate synthetic spectra by varying several parameters, the model generated spectra are then matched with the observed emission line spectra obtained at two epochs. We obtain the best fit model parameters through the χ 2 minimization technique. Our model results fit well with observed optical and near-infrared spectra. The best-fit model parameters are compatible with a hot white dwarf source with T BB of 5.5 -5.8 × 10 5 K and roughly constant a luminosity of 6 -8 × 10 36 ergs s −1 . From the analysis we find the following abundances (by number) of elements with respect to solar: He/H = 1.8 ± 0.1, N/H = 12.0 ± 1.0, O/H = 1.0 ± 0.4, Ne/H = 1.5 ± 0.1, Si/H = 0.4 ± 0.1, Fe/H = 3.2 ± 0.2, Ar/H = 5.1 ± 0.1, and Al/H = 1.0 ± 0.1, all other elements were set at the solar abundance. This shows the ejecta are significantly enhanced, relative to solar, in helium, nitrogen, neon, iron and argon. Using the obtained parameter values, we estimate an ejected mass in the range of 3.4 -4.9 × 10 −6 M ⊙ which is consistent with observational results.

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Section: Estimation Of the Ejecta Masssupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Abundance analysis of the recurrent nova RS Ophiuchi (2006 outburst)

Das

Mondal

2015

New Astronomy

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“…Shocks themselves may be apparently absent in systems where expected to appear, such as in the symbiotic Nova Sco 2014 (Joshi et al 2015). The speed of the shocks and the angle at which the shocks are viewed may play a large part in determining whether γ-rays are detected in nearby novae (Metzger et al 2015;Dmitrievich Vlasov et al 2016). If this were the case, it could explain systems such as the clearly shock-powered yet γ-ray faint V5589 Sgr.…”

Section: Connection To γ-Ray Producing Novaementioning

confidence: 99%

“…These shocks can be caused by collisions with pre-existing circumstellar material (eg., V407 Cyg, V745 Sco, and RS Oph; Bode et al 2006;Das et al 2006; interactions between multiple flows from the same eruption (eg., V959 Mon, T Pyx, V382 Vel; Mukai & Ishida 2001;Nelson et al 2014;. Radio monitoring of novae, especially when combined with observations at other frequencies, provides a powerful tool for understanding the evolution of nova eruptions and examining shocks within the ejecta.…”

Section: Introductionmentioning

confidence: 99%

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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“…Numerous works studied the new outburst in multiple spectral regions, e.g., in X-rays Ness et al 2007;Vaytet et al 2007), in optical ), in infrared (Das et al 2006;Chesneau et al 2007;Evans et al 2007a,b;Lane et al 2007), and in radio wavelength . Some theoretical work on the explosion was carried out (e.g., Hachisu et al 2006).…”

Section: Introductionmentioning

confidence: 99%