0.8–2.5 Micron Spectroscopy of Nova Ophiuchi 1998

Lynch, D. K.; Rudy, R. J.; Mazuk, S.; Puetter, R. C.

doi:10.1086/309453

Cited by 47 publications

(46 citation statements)

References 22 publications

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“…All line strengths in this figure panel are normalized to Paβ. The model fit from Lynch et al (2000), using the same parameters for the gas as described above, do not however give as good a fit as before. The ratio of Paγ to Paβ is depressed in the model vis-à-vis the observed value.…”

Section: Resultsmentioning

confidence: 91%

“…However, the effects of such blending if present and accounted for, will only move the observed data points farther away from the model fit. This discrepancy in the model results can be explained if the geometry of the emitting regions is rather more complex than assumed by Lynch et al (2000). Further as stated by them, their model is meant to be simple and illustrative rather than an accurate model of the formation of lines in a realistic emission-line region.…”

Section: Resultsmentioning

confidence: 98%

“…The Case B line strengths, shown by the dashed line, are seen to deviate significantly from the observed values indicating optical depth effects. Lynch et al (2000) have developed a model to explain such deviations and have shown that the relatively larger intensities of the higher members of the Pa and Br series are because of emission from high-density or optically thick emission-line gas. Increased strength in the higher lines occurs when the level populations become thermalized at high densities (n e ≥ 10×10 10 cm −3 ) or at large optical depths.…”

Section: Resultsmentioning

confidence: 99%

“…We tried model fits for other combinations of the parameters n e , T and τ . Lynch et al (2000) give data for combinations of n e = 6×10 10 and 6×10 11 cm −3 ; T = 5×10 3 , 1.0×10 4 , 1.5×10 4 K; and τ = 10, 100 and 1000. However, we found that the excessive strength of the higher lines visa-vis the lower lines like Brγ (just the opposite of Case B predictions) can only be explained by invoking large optical depth values for the parameter τ .…”

Section: Resultsmentioning

confidence: 99%

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Near infra-red and optical spectroscopy of Delta Scorpii

Banerjee

Janardhan

Ashok

2001

A&A

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Abstract. Spectroscopic observations of δ Sco in the near IR and optical wavelengths, obtained shortly after its recent periastron passage are reported. The IR spectra are dominated by the HI Paschen and Brackett lines. An IR excess is seen which can be attributed to free-free emission from a circumstellar shell. The observed Paschen and Brackett line intensities deviate significantly from Case B predictions and indicate optical depth effects. These effects are modeled. The overall spectral behaviour of δ Sco at present is that of a typical Be star.

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Section: Resultsmentioning

confidence: 91%

Section: Resultsmentioning

confidence: 98%

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

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Near infra-red and optical spectroscopy of Delta Scorpii

Banerjee

Janardhan

Ashok

2001

A&A

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“…Similar optical depth effects in the Br lines, due to high plasma densities during the early stages after outburst, are common and have been seen in several other novae, e.g. Nova Oph 1998 (Lynch et al 2000 Following the formalism of Hummer & Storey (1987) and Storey & Hummer (1995), the optical depth at the Brγ line centre is given by…”

Section: Case B Analysismentioning

confidence: 53%

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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RXTE andXMMobservations of intermediate polar candidates

Butters

Norton

Mukai

et al. 2010

A&A

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Aims. We aim to determine the credentials of nine candidate intermediate polars in order to confirm whether or not they are magnetic cataclysmic variables. Methods. Frequency analysis of RXTE and XMM data was used to search for temporal variations that could be associated with the spin period of the magnetic white dwarf. X-ray spectral analysis was carried out to characterize the emission and absorption properties of each target.Results. The hard X-ray light curve of V2069 Cyg shows a pulse period of 743.2 s, and its spectrum is fit by an absorbed bremsstrahlung model with an iron line, confirming this to be a genuine intermediate polar. The hard X-ray light curve of the previously confirmed intermediate polar IGR J00234+6141 is shown to be consistent with the previous low-energy X-ray detection of a 563.5 s pulse period. The likely polar IGR J14536-5522 shows no coherent modulation at the previously identified period of 3.1 h, but does exhibit a clear signal at periods likely to be harmonically related to it. Whilst our RXTE observations of RX J0153.3+7447, Swift J061223.0+701243.9, V436 Car, and DD Cir are largely too faint to give any definitive results, the observations of IGR J16167-4957 and V2487 Oph show some characteristics of intermediate polars, and these objects remain good candidates. Conclusions. We confirmed one new hard X-ray selected intermediate polar from our sample, V2069 Cyg.

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0.8–2.5 Micron Spectroscopy of Nova Ophiuchi 1998

Cited by 47 publications

References 22 publications

Near infra-red and optical spectroscopy of Delta Scorpii

Near infra-red and optical spectroscopy of Delta Scorpii

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

RXTE andXMMobservations of intermediate polar candidates

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