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Geballe, T. R.; Evans, A.; Smalley, B.; Tyne, V. H.; Eyres, S. P. S.

doi:10.1023/a:1014683521291

Cited by 31 publications

(45 citation statements)

References 2 publications

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“…The observed spectra together with observational details were presented by Eyres et al (1998) and the July spectrum is also shown in Geballe et al (2002). The resolutions of these spectra as presented here are 1.4 nm (0.0014 µm) at 1.02-1.35 µm and 2.8 nm (0.0028 µm) at 1.42-2.52 µm.…”

Section: Have Found Peculiarities Similar Tomentioning

confidence: 53%

“…1 the principal features formed by the molecular species C 2 , CO, and CN are displayed as separate spectra. Atomic features are also shown, as these are also present in Sakurai's Object (see Eyres et al 1998;Geballe et al 2002). As in the optical spectrum , absorption of only a few molecular species accounts for the main features in the IR spectrum.…”

Section: Principal Spectral Featuresmentioning

confidence: 81%

“…The new dust would be expected to have been close to the star and thus quite hot. Indeed the full 1-5 µm spectrum from 1998 (e.g., Geballe et al 2002) shows that the excess peaked close to 3 µm, indicating a mean dust temperature close to 1000 K at that time. The dust must have been hotter (and closer) in 1997; this is supported by the data from 1997 (Eyres et al 1998;Geballe et al 2002) which show that the continuum flux density decreased monotonically with wavelength in the observed wavelength range, 1-4 µm, at that time.…”

Section: Discussionmentioning

confidence: 97%

“…The accuracy of the determination of log N(C) is limited mainly by the quality of the molecular line list. The effective temperatures that best fit the 1.0-2.0 µm spectra in 1997 April and July are 5500 ± 200 K and 5250 ± 200 K, respectively, indicating that the cooling evidenced by the dramatic spectral changes seen between 1996 and 1997 (e.g., Geballe et al 2002) continued in 1997. Our estimated uncertainties in the above temperatures are rather large, despite the comparatively good fits to the observed spectra, because of questions concerning abundances, non-sphericity effects, and dynamical phenomena, and because of contamination of the spectra by dust emission (see below).…”

Section: Changes Between 1997 April 21 and July 13mentioning

confidence: 95%

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Models of infrared spectra of Sakurai's Object (V4334 Sgr) in 1997

Pavlenko

Geballe²

2002

A&A

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Abstract. Theoretical spectral energy distributions computed for a grid of hydrogen-deficient and carbon-rich model atmospheres have been compared with the observed infrared (1-2.5 µm) spectra of V4334 Sgr (Sakurai's Object) on 1997 April 21 and July 13. The comparison yields an effective temperature of T eff = 5500 ± 200 K for the April date and T eff = 5250 ± 200 K for July. The observed spectra are well fitted by Asplund et al. (1999) abundances, except that the carbon abundance is higher by 0.3 dex. Hot dust produces significant excess continuum at the long wavelength ends of the 1997 spectra.

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Section: Have Found Peculiarities Similar Tomentioning

confidence: 53%

Section: Principal Spectral Featuresmentioning

confidence: 81%

Section: Discussionmentioning

confidence: 97%

Section: Changes Between 1997 April 21 and July 13mentioning

confidence: 95%

See 2 more Smart Citations

Models of infrared spectra of Sakurai's Object (V4334 Sgr) in 1997

Pavlenko

Geballe²

2002

A&A

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“…However, the nearinfrared flux from V838 Mon, which also was very strong after the January eruption and underwent large fluctuations during the subsequent outbursts in the first few months of 2002, has only declined slowly since then. The optical and infrared behavior of V838 Mon, coupled with the presence of P Cygni and (later) inverse P Cygni profiles (Zwitter & Munari 2002;Geballe et al 2002;Kipper et al 2004;Rushton et al 2005a) suggest that considerable material was ejected from the star, but that some of the material was being returned. A prominent light echo surrounding V838 Mon (Hemden et al 2002) appeared shortly after the second outburst.…”

Section: Introductionmentioning

confidence: 98%

Infrared spectroscopy of carbon monoxide in V838 Monocerotis during 2002–2006

Geballe

Rushton

Eyres

et al. 2007

A&A

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Aims. We report spectra of the overtone and fundamental bands of CO in the eruptive variable V838 Mon, which trace the recent evolution of the star and allow its ejecta to be characterized. Methods. The data were obtained at the United Kingdom Infrared Telescope on fourteen nights from 2002 January, shortly after the first outburst of the star, to 2006 April. Results. Although the near-infrared stellar spectrum superficially resembled a cool supergiant after both the first and third of its outbursts in 2002, its infrared "photosphere" at that time consisted of highly blueshifted gas that was moving outward from the original stellar surface. A spectrum obtained during the third outburst reveals a remarkable combination of emission and absorption in the CO first overtone bands. The most recent observations show a composite spectrum that includes a stellar-like photosphere at a temperature similar to that seen just after the initial outburst, but at a radial velocity redshifted by 15 km s −1 relative to the stellar velocity determined from SiO maser emission, suggesting that the atmosphere is now contracting. Three shell components, corresponding to expansion velocities of 15, 85, and 145 km s −1 , also are present, but absorption is seen at all expansion velocities out to 200 km s −1 . Weak absorption features of fundamental band lines of 13 CO have been detected. However, the large uncertainty in the value of 12 C/ 13 C does not constrain the evolutionary status of the progenitor.

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CK Vul: reborn perhaps, but not hibernating

Evans

Loon

Zijlstra³

et al. 2002

Monthly Notices of the Royal Astronomical Society

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A B S T R A C TIt has been claimed that CK Vul (the remnant of Nova Vul 1670) may be the oldest recovered 'old nova' and as such provides evidence in support of the hibernation scenario for classical nova systems. However this interpretation has been challenged. We present 450-and 850-mm photometry of CK Vul which cast further doubt on its old nova status. It displays a large far infrared-submillimetre flux excess, inconsistent with the properties of an old nova. Furthermore, IRAS images show that CK Vul is located in a 'cavity' in the infrared emission, a feature often associated with planetary nebulae. It seems more likely that CK Vul -and hence Nova Vul 1670 -is (like V605 Aql and V4334 Sgr) an evolved star in the throes of a final thermal pulse.

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Cited by 31 publications

References 2 publications

Models of infrared spectra of Sakurai's Object (V4334 Sgr) in 1997

Models of infrared spectra of Sakurai's Object (V4334 Sgr) in 1997

Infrared spectroscopy of carbon monoxide in V838 Monocerotis during 2002–2006

CK Vul: reborn perhaps, but not hibernating

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