On the Raman O VI and related lines in classical novae

Shore, Steven N.; Aquino, I. De Gennaro; Scaringi, Simone; Winckel, H. Van

doi:10.1051/0004-6361/201424786

Cited by 13 publications

(19 citation statements)

References 15 publications

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“…Nussbaumer et al (1989) and Schmid (1989) were the first to propose that an emission band at ∼6830 Å could be due to the Raman (1928) scattering of the O VI resonance doublet (1032/1038 Å) by neutral hydrogen. As Shore et al (2014) also point out, such Raman features are unlikely to be formed in the ejecta of MS-or SG-novae, but such features have been observed in the spectra of RG-novae (most notably, RS Oph; Joy & Swings 1945;Wallerstein & Garnavich 1986;Iijima 2009) and are common features of the wider group of symbiotic stars (Allen 1980). We note that the weaker Raman band at 7088 Å would be blended with the strong He I emission at 7065 Å.…”

Section: Multi-eruption Combined Visible Spectrummentioning

confidence: 54%

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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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Section: Multi-eruption Combined Visible Spectrummentioning

confidence: 54%

“…As noted by Shore et al (2014), a possible interpretation of this line is "simply" emission from C I (6830 Å), especially in CNe. However, we also note that other (typically stronger; see Kramida et al 2015) C I lines (e.g., 6014 and 7115 Å) are not seen in the combined spectrum.…”

Section: Multi-eruption Combined Visible Spectrummentioning

confidence: 87%

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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“…Four ionization stages were available for C (C • -C +3 ) (C I profiles from the earliest spectra are presented in Shore et al (2014) and de Gennaro Aquino et al (2015) and N (N + -N +4 ) during the epochs of simultaneous FIES and STIS coverage. This spectral development is shown in Figs.…”

Section: Discussionmentioning

confidence: 99%

“…It has been detected in the range γ-rays A&A 590, A123 (2016) (Ackermann et al 2014) through centimeter radio (ATel 5298,5376). A study of the carbon spectrum in V339 del was published in Shore et al (2014). A high resolution atlas of the first four months of the outburst, covering 3800−8800 Å, has been published by De Gennaro Aquino et al (2015) and a discussion of the infrared development by Gehrz et al (2015).…”

Section: Introductionmentioning

confidence: 99%

The panchromatic spectroscopic evolution of the classical CO nova V339 Delphini (Nova Del 2013) until X-ray turnoff

Shore

Mason

Schwarz

et al. 2016

A&A

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Context. Classical novae are the product of thermonuclear runaway-initiated explosions occurring on accreting white dwarfs. Aims. V339 Del (Nova Delphinus 2013) was one of the brightest classical novae of the last hundred years. Spectroscopy and photometry are available from γ-rays through infrared at stages that have frequently not been observed well. The complete data set is intended to provide a benchmark for comparison with modeling and for understanding more sparsely monitored historical classical and recurrent novae. This paper is the first in the series of reports on the development of the nova. We report here on the early stages of the outburst, through the X-ray active stage. Methods. A time sequence of optical, flux calibrated high resolution spectra was obtained with the Nordic Optical Telescope (NOT) using FIES simultaneously, or contemporaneously, with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope during the early stages of the outburst. These were supplemented with Mercator/HERMES optical spectra. High resolution IUE ultraviolet spectra of OS And 1986, taken during the Fe curtain phase, served as a template for the distance determination. We used standard plasma diagnostics (e.g., [O III] and [N II] line ratios, and the Hβ line flux) to constrain electron densities and temperatures of the ejecta. Using Monte Carlo modeling of the ejecta, we derived the structure, filling factor, and mass from comparisons of the optical and ultraviolet line profiles. Results. We derive an extinction of E(B − V) = 0.23 ± 0.05 from the spectral energy distribution, the interstellar absorption, and H I emission lines. The distance, about 4−4.5 kpc, is in agreement with the inferred distance from near infrared interferometry. The maximum velocity was about 2500 km s −1 , measured from the UV resonance and optical profiles. The ejecta showed considerable fine structure in all transitions, much of which persisted as emission knots. The line profiles were modeled using a bipolar conical structure for the ejecta within a relatively restricted range of parameters. For V339 Del, we find that an inclination to the line of sight of about 35• −55• , an opening angle of 60 • −80• , and an inner radius ∆R/R(t) ≈ 0.3 based on v rad,max matches the permitted and intercombination lines. The filling factor is f ≈ 0.1, and the derived range in the ejecta mass is (2−3) × 10 −5 M .

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“…They determined the ejected mass to be a few × 10 −4 M . Skopal et al also reported the emergence of Raman-scattered O VI λ = 1032, 1038 Å at around 6825 Å (but see Shore et al 2014, for a more plausible counter-interpretation in terms of emission by C I). Shore et al (2016) have undertaken a multiwavelength study of V339 Del, including X-ray data obtained with Swift, UV with the Hubble Space Telescope and ground-based optical observations.…”

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

confidence: 98%

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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On the Raman O VI and related lines in classical novae

Cited by 13 publications

References 15 publications

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

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

The panchromatic spectroscopic evolution of the classical CO nova V339 Delphini (Nova Del 2013) until X-ray turnoff

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

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