Photometric evolution, orbital modulation and progenitor of Nova Mon 2012

Munari, U.; Dallaporta, S.; Castellani, F.; Valisa, P.; Frigo, A.; Chomiuk, Laura; Ribeiro, V. A. R. M.

doi:10.1093/mnras/stt1340

Cited by 35 publications

(55 citation statements)

References 28 publications

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“…The nova is most likely at a distance of about 1.4 kpc (Linford et al 2015;Munari et al 2013;Ribeiro et al 2013) although a larger distance, of 3.6 kpc, has been proposed (Shore et al 2013). It is effected by a large column density of neutral hydrogen with 5.9-7.4 ×10 21 cm −2 (measured towards the nova direction according to the HEASARC nH online tool, see references therein).…”

Section: V959 Mon a Nova Discovered As A Gamma-ray Sourcementioning

confidence: 97%

“…The decrease in optical magnitude currently continues, after a slow decline by only about 7 magnitudes in the first 33 months. Munari et al (2013) noticed that the only change in the rate of optical decline was a break around the time the nova turned off as a supersoft X-ray source, in January 2013 (Page et al 2013). …”

Section: V959 Mon a Nova Discovered As A Gamma-ray Sourcementioning

confidence: 99%

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Chemical and Physical Parameters From X-Ray High-Resolution Spectra of the Galactic Nova V959 Mon

Peretz

Orio

Behar

et al. 2016

ApJ

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Two observations of V959 Mon, done using the Chandra X-ray gratings during the late outburst phases (2012 September and December), offer extraordinary insight into the physics and chemistry of this Galactic ONe nova. The X-ray flux was 1.7 × 10 −11 erg cm −2 s −1 and 8.6 × 10 −12 erg cm −2 s −1 , respectively at the two epochs. The first result, coupled with electron density diagnostics and compared with published optical and ultraviolet observations, indicates that most likely in 2012 September the X-rays originated from a very small fraction of the ejecta, concentrated in very dense clumps. We obtained a fairly good fit to the September spectrum with a model of plasma in collisional ionization equilibrium (CIE) with two components; one at a temperature of 0.78 keV, associated with flat-topped and asymmetrical emission lines, blueshifted by 710-930 km s −1 ; the other at a temperature of 4.5 keV, mostly contributing to the high-energy continuum. However, we cannot rule out a range of plasma temperatures between these two extremes; we also modeled the spectrum as a static cooling flow, but the available models and the data quality are not adequate yet to differentiate between the two-component fit and a smoothly varying temperature structure. In December, the central white dwarf (WD) became visible in X-rays. We estimate an effective temperature of 680,000 K, consistent with a WD mass ≥1.1 M . The WD flux is modulated with the orbital period, indicating high inclination, and two quasi-periodic modulations with hour timescales were also observed. No hot plasma component with temperature above 0.5 keV was observed in December, and the blueshifted component cooled to kT 0.45 keV. Additionally, new emission lines due to a much cooler plasma appeared, which were not observed two months earlier. We estimate abundances and yields of elements in the nova wind that cannot be measured in the optical spectra and confirm the high Ne abundance previously derived for this nova. We also find high abundance of Al, 230 times the solar value, consistently with the prediction that ONe novae contribute to at least 1/3rd of the Galactic yield of 26 Al.

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Section: V959 Mon a Nova Discovered As A Gamma-ray Sourcementioning

confidence: 97%

Section: V959 Mon a Nova Discovered As A Gamma-ray Sourcementioning

confidence: 99%

Chemical and Physical Parameters From X-Ray High-Resolution Spectra of the Galactic Nova V959 Mon

Peretz

Orio

Behar

et al. 2016

ApJ

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“…Interstellar absorption line measurements toward Nova Mon 2012 were reported by Munari et al (2012) who, using the E(B − V) vs. equivalent width calibration for a hydrogen column density, N H . However, the UV spectra have been determinative in extending the velocity range of the absorption features, especially indicating that the Na I had a weak component at high (positive) radial velocity (Fig.…”

Section: Determination Of Extinction and Integrated Fluxes And Comparmentioning

confidence: 99%

The spectroscopic evolution of theγ-ray emitting classical nova Nova Mon 2012

Shore¹,

Aquino²,

Schwarz³

et al. 2013

A&A

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Among the classical novae, the ONe subgroup, distinguished by their large overabundance of neon, are thought to occur on the most massive white dwarfs. Nova Mon 2012 was the first classical nova to be detected as a high energy γ-ray transient, by Fermi-LAT, before its optical discovery. The first optical spectra obtained about 55 days after γ-ray peak, were strikingly similar to the ONe class after the transition to the nebular (optically thin) spectrum. The current paper presents our subsequent optical and ultraviolet observations. A time sequence of optical echelle spectra (3700-7400Å) with the Nordic Optical Telescope (NOT) began on 2012 Aug. 16, immediately following the optical announcement, and are continuing. The nova was observed almost simultaneously with the NOT on 2012 Nov. 21, with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope at medium echelle resolution (1150-3050Å) on Nov. 20, and with the CHIRON CTIO/SMARTS echelle spectrograph at medium resolution (4500-8900Å) on Nov. 22. We use plasma diagnostics (e.g. [O III] and Hβ line flux) to constrain electron densities and temperatures, and the filling factor, for the ejecta. Using Monte Carlo modeling, we derive the structure from comparisons to the optical and ultraviolet line profiles. We also compare observed fluxes for Nova Mon 2012 with those predicted by photoionization modeling with Cloudy using element abundances derived for other ONe novae, the parameters derived from the line profile modeling and multiwavelength continuum measurements. Nova Mon 2012 is confirmed as an ONe nova first observed spectroscopically in the nebular stage. We derive an extinction of E(B-V)=0.85±0.05 and hydrogen column density N H ≈ 5 × 10 21 cm −2 . The corrected continuum luminosity is nearly the same in the entire observed energy range compared to V1974 Cyg, V382 Mon, and Nova LMC 2000 at the same epoch after outburst. The distance, about 3.6 kpc, is quite similar to V1974 Cyg, suggesting that it would have been equally bright had it been observed at maximum light. The same applies to the line profiles. These can be modeled using an axisymmetric conical -bipolargeometry for the ejecta with various inclinations of the axis to the line of sight, i, and ejecta inner radii. For Nova Mon 2012, we find that 60 ≤ i ≤ 80 degrees, an opening angle of ≈70 o , and an inner radius ∆R/R(t) ≈ 0.4 matches the permitted and intercombination lines while the forbidden lines require a less filled structure. The filling factor is f ≈ 0.1 − 0.3, although it may be lower based on the structures observed in the emission line profiles, implying an ejecta mass ≤ 6 × 10 −5 M ⊙ . The abundances are similar to, but not identical to, V1974 Cyg and V382 Vel. In particular, Ne and Mg are apparently more abundant in Nova Mon 2012. The ONe novae appear to comprise a single physical class with bipolar high mass ejecta, similarly enhanced abundances, and a common spectroscopic evolution within a narrow range of luminosities. The spectral evolution does not require c...

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“…(1) Crampton et al (1987); (2 Kahabka (1996); (9) Tomov et al (1998) Ribeiro et al (2013b); (17) Munari et al (2013); (18) Bos et al (2001); (19) Barsukova & Goranskii (2003); (20) Hachisu et al (2004); (21) Iijima & Esenoglu (2003); (22) Ribeiro et al (2011);(23) Helton et al (2008); (24) Dobrotka et al (2008); (25) Sala et al (2008); (26) Lyke & Campbell (2009); (27) Goranskij et al (2007); (28) Shore et al (2003); (29) Della Valle et al (2002); (30) Dobrzycka & Kenyon (1994); (31) Ribeiro et al (2009);(32) Bode (1987); (33) Barry et al (2008); (34) Schaefer (1990); (35) Thoroughgood et al (2001); (36) Schaefer (2010); (37) Chesneau et al (2011);(38) Uthas et al (2010); (39) Sokoloski et al (2013); …”

Section: Referencesmentioning

confidence: 99%

Obscuration effects in super-soft-source X-ray spectra

Ness

Osborne

Henze

et al. 2013

A&A

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Context. Super-soft-source (SSS) X-ray spectra are blackbody-like spectra with effective temperatures ∼3−7 × 10 5 K and luminosities of 10 35−38 erg s −1 . Grating spectra of SSS and novae in outburst that show SSS type spectra display atmospheric absorption lines. Radiation transport atmosphere models can be used to derive physical parameters. Blue-shifted absorption lines suggest that hydrostatic equilibrium is an insufficient assumption, and more sophisticated models are required. Aims. In this paper, we bypass the complications of spectral models and concentrate on the data in a comparative, qualitative study. We inspect all available X-ray grating SSS spectra to determine systematic, model-independent trends. Methods. We collected all grating spectra of conventional SSS like Cal 83 and Cal 87 plus observations of novae during their SSS phase. We used comparative plots of spectra of different systems to find common and different features. The results were interpreted in the context of system parameters obtained from the literature.

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Photometric evolution, orbital modulation and progenitor of Nova Mon 2012

Cited by 35 publications

References 28 publications

Chemical and Physical Parameters From X-Ray High-Resolution Spectra of the Galactic Nova V959 Mon

Chemical and Physical Parameters From X-Ray High-Resolution Spectra of the Galactic Nova V959 Mon

The spectroscopic evolution of theγ-ray emitting classical nova Nova Mon 2012

Obscuration effects in super-soft-source X-ray spectra

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