A model for the outburst of nova RS Ophiuchi in 1985

Bode, M. F.; Kahn, F. D.

doi:10.1093/mnras/217.1.205

Cited by 95 publications

(109 citation statements)

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“…This is surprising since the H-band brightness faded by a factor of 110 during this time. This result is discordant with the generic prediction of Evans et al (1988), who interpreted the IR light curve in terms of the time evolution of postshock gas at 10 5 K moving at the speed of the contact discontinuity, 1400 km s Ϫ1 (following the earlier work by Bode & Kahn 1985). This model requires the IR emission to be seen expanding at a rate of ∼1.0 mas day Ϫ1 (assuming a distance of 1.6 kpc), an interpretation that is now ruled out.…”

Section: Discussionsupporting

confidence: 59%

“…Second, the mass-losing companion for RS Oph is a red giant (RG) with a wind, providing a high-density medium for accretion onto the WD as well as for the exploding blast wave to interact with. Bode & Kahn (1985) have produced the most successful model for recurrent novae, drawing a clear analogy to extragalactic supernovae and explaining the radio and X-ray light curves in this context. Evans et al (1988) were the first to study in detail the IR time evolution of a recurrent nova.…”

Section: Introductionmentioning

confidence: 99%

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No Expanding Fireball: Resolving the Recurrent Nova RS Ophiuchi with Infrared Interferometry

Monnier

Barry

Traub

et al. 2006

ApJ

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Following the recent outburst of the recurrent nova RS Oph on 2006 February 12, we measured its near-infrared size using the IOTA, Keck, and PTI Interferometers at multiple epochs. The characteristic size of ∼3 mas hardly changed over the first 60 days of the outburst, ruling out currently popular models whereby the near-infrared emission arises from hot gas in the expanding shock. The emission was also found to be significantly asymmetric, evidenced by nonzero closure phases detected by IOTA. The physical interpretation of these data depends strongly on the adopted distance to RS Oph. Our data can be interpreted as the first direct detection of the underlying RS Oph binary, lending support to the recent "reborn red giant" models of Hachisu & Kato. However, this result hinges on an RS Oph distance of Շ540 pc, in strong disagreement with the widely adopted distance of ∼1.6 kpc. At the farther distance, our observations imply instead the existence of a nonexpanding, dense, and ionized circumbinary gaseous disk or reservoir responsible for the bulk of the near-infrared emission. Longer baseline infrared interferometry is uniquely suited to distinguish between these models and to ultimately determine the distance, binary orbit, and component masses for RS Oph, one of the closest known (candidate) Type 1a supernova progenitor systems.

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Section: Discussionsupporting

confidence: 59%

Section: Introductionmentioning

confidence: 99%

No Expanding Fireball: Resolving the Recurrent Nova RS Ophiuchi with Infrared Interferometry

Monnier

Barry

Traub

et al. 2006

ApJ

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“…A series of visible spectra was collected, the first just 1.27 days after the eruption, and these showed modest expansion velocities ( =  v 2600 100 ej km s −1 ) for such a fast nova, which significantly decreased over the course of just a few days. Such an inferred deceleration is reminiscent of the interaction of the ejecta with pre-existing circumbinary material (such as the red giant wind in the case of RS Oph; Bode & Kahn 1985;Bode et al 2006).…”

Section: A Remarkable Rnmentioning

confidence: 99%

“…Similar "decelerations" have been seen in a number of RNe-most notably, in RSOph (Dufay et al 1964;Iijima 2009)-and have been linked to the physical deceleration of the ejecta as they interact with significant circumbinary material (in the case of RS Oph, the red giant wind; Pottasch 1967; Bode et al 2006;Evans et al 2007). Bode & Kahn (1985) described the standard three-phase model of the interaction of the ejecta with a shocked r 1 2 density profile stellar wind. PhaseI is the early stage of the interaction, and the ejecta are still imparting energy to the shocked wind, and the reverse shock, running into the ejecta, remains important.…”

Section: Ejecta Deceleration and Eruption Environmentmentioning

confidence: 99%

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

Darnley

Henze

Bode

et al. 2016

ApJ

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The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of =  P 351 13 rec days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground-and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swiftobservatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28±0.12 UT. The 2013-2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities ∼13,000 km s −1 ,

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“…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%

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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A model for the outburst of nova RS Ophiuchi in 1985

Cited by 95 publications

References 0 publications

No Expanding Fireball: Resolving the Recurrent Nova RS Ophiuchi with Infrared Interferometry

No Expanding Fireball: Resolving the Recurrent Nova RS Ophiuchi with Infrared Interferometry

M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

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

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