Multiwavelength analyses of the extraordinary nova LMC 1991

Schwarz, Greg J.; Shore, Steven N.; Starrfield, S.; Hauschildt, P. H.; Valle, M. Della; Baron, Edward

doi:10.1046/j.1365-8711.2001.03960.x

Cited by 90 publications

(106 citation statements)

References 55 publications

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“…et al 2015 and suffered a large absorbing column density. The only other nova given in Schwarz et al (2001) with both of these characteristics is V1663 Aql, a nova that was also never detected as a super-soft source. Another possible explanation for the lack of soft X-rays from V1324Sco is that it occurred on a low-mass white dwarf, and the white dwarf photosphere was never hot enough to emit X-rays, instead peaking in the UV band (Sala & Hernanz 2005;Wolf et al 2013).…”

Section: X-ray Datamentioning

confidence: 98%

“…Note that, along with the peculiar lack of hard X-rays from nonthermal particle acceleration, there was also a lack of soft X-rays, which are often seen at later times as the ejecta clear away and reveal the central hot white dwarf (e.g., Schwarz et al 2001). However, V1324 Sco was both distant (6.5 kpc; Finzell Table 3 for details on the telescopes and instruments used for the different spectra.…”

Section: X-ray Datamentioning

confidence: 99%

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A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Finzell

Chomiuk

Metzger

et al. 2018

ApJ

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It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanisms involved in the production ofgamma-rays are still not well understood. We present here a comprehensive multiwavelength data set-from radio to X-rays-for the most gamma-ray-luminous classical nova to date, V1324 Sco. Using this data set, we show that V1324 Sco is a canonical dusty Fe II-type nova, with a maximum ejecta velocity of 2600 km s −1 and an ejecta mass of a few´-10 5  M . There is also evidence for complex shock interactions, including a double-peaked radio light curve which shows high brightness temperatures at early times. To explore why V1324Sco was so gamma-ray luminous, we present a model of the nova ejecta featuring strong internal shocks and find that higher gamma-ray luminosities result from higher ejecta velocities and/or mass-loss rates. Comparison of V1324Sco with other gamma-ray-detected novae does not show clear signatures of either, and we conclude that a larger sample of similarly well-observed novae is needed to understand the origin and variation of gamma-rays in novae.

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Section: X-ray Datamentioning

confidence: 98%

Section: X-ray Datamentioning

confidence: 99%

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Finzell

Chomiuk

Metzger

et al. 2018

ApJ

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“…Our first observation, JD 55 667, was one day after the discovery and showed a fireball spectrum (see, e.g., Schwarz et al 2001) dominated by P Cygni profiles of the H I Balmer lines (Figs. 2 and B.1), He I, and and He II, for which the absorption extended without a terminal edge to ≈2500 km s −1 ; Fig.…”

Section: Discrete Absorption Featuresmentioning

confidence: 86%

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

Shore

Augusteijn

Ederoclite

et al. 2011

A&A

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Aims. We aim to derive the physical properties of the recurrent nova T Pyx and the structure of the ejecta during the early stages of expansion of the 2011 outburst. Methods. The nova was observed with high resolution spectroscopy (R ≈ 65 000), from one day after discovery of the outburst and until the last visibility of the star at the end of May 2011. The interstellar absorption lines of Na I, Ca II, CH, CH + , and archival H I 21 cm emission line observations were used to determine a kinematical distance. Interstellar diffuse absorption features have been used to determine the extinction independent of previous assumptions. Sample Fe-peak line profiles show the optical depth and radial velocity evolution of the discrete components. Results. We propose a distance to T Pyx ≥ 4.5 kpc, with a strict lower limit of 3.5 kpc (the previously accepted distance). We derive an extinction, E(B − V) ≈ 0.5 ± 0.1, that is higher than previous estimates. The first observation, Apr. 15, displayed He I, He II, C III, and N III emission lines and a maximum velocity derived from the P Cyg profiles of the Balmer and He I lines of ≈2500 km s −1 that is characteristic of the fireball stage. These ions were undetectable in the second spectrum, Apr. 23, and we use the recombination time to estimate the mass of the ejecta, 10 −5 f M for a filling factor f . Numerous absorption-line systems were detected in the Balmer, Fe-peak, Ca II, and Na I lines, mirrored in broader emission-line components, that showed an "accelerated" displacement in velocity. We also show that the time sequence of these absorptions, which are common to all lines and arise only in the ejecta, can be described by a recombination front moving outward in the expanding gas without either a stellar wind or circumstellar collisions. By the end of May, the ejecta were showing signs of turning optically thin in the ultraviolet.

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“…V1187 Sco showed many emission lines of all three neutral elements. Most classical novae show many N i and C i emission lines in the infrared because nitrogen is always enhanced regardless of WD type (Schwarz et al 2001;Schwarz 2002;Vanlandingham et al 1996Vanlandingham et al , 1997Vanlandingham et al , 1999Vanlandingham et al , 2005. The Ly -fluoresced O i lines were very strong throughout the observing period (Fig.…”

Section: Near-ir Spectra (Days 10-58)mentioning

confidence: 94%

Early Infrared Spectral Development of V1187 Scorpii (Nova Scorpii 2004 No. 2)

Lynch¹,

Woodward²,

Geballe³

et al. 2006

ApJ

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We report on an unprecedented infrared time series of spectra of V1187 Sco, a very fast ONeMg nova. The observations covered a 56 day period (2004 August 6-September 30) starting 2 days after the nova's peak brightness. Time evolution of the spectra revealed changing line strengths and profiles on timescales of less than a day to weeks as the nova evolved from early postmaximum to early coronal phases. When our ground-based optical and Spitzer Space Telescope data were combined, the wavelength coverage of 0.38-36 m allowed an accurate spectral energy distribution to be derived when it was about 6 weeks after outburst. Developing double structure in the He i lines showed them changing from narrow to broad in only a few days. Using the O i lines in combination with the optical spectra, we derived a reddening of E(B À V ) ¼ 1:56 AE 0:08 and a distance of 4:9 AE 0:5 kpc. Modeling of the ejected material strongly suggested that it was geometrically thick with ÁR/R ¼ 0:8 0:9 (more of a wind than a shell) and a low filling factor of order a few percent. The line shapes were consistent with a cylindrical jet, bipolar, or spherical Hubble flow expansion with a maximum speed of about À3000 km s À1 . The central peak appeared to be more associated with the spherical component, while the two peaks (especially in H ) suggested a ring with either a lower velocity component or with its axis inclined to the line of sight.

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Multiwavelength analyses of the extraordinary nova LMC 1991

Cited by 90 publications

References 55 publications

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst

Early Infrared Spectral Development of V1187 Scorpii (Nova Scorpii 2004 No. 2)

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