The 2000 outburst of the recurrent nova CI Aquilae: Optical spectroscopy

Kiss, L. L.; Thomson, James Robertson; Ogłoza, W.; Fürész, Gábor; Sziladi, K.

doi:10.1051/0004-6361:20010015

Cited by 31 publications

(58 citation statements)

References 20 publications

(43 reference statements)

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“…The spectral evolution in the optical region of this object during the outburst in 2000 was reported in some previous works Calibrated high-resolution spectra are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/544/A26 (Burlak & Esipov 2001;Kiss et al 2001;Matsumoto et al 2001). Lynch et al (2004) performed a detailed analysis for the nearinfrared spectra obtained in 2000 and 2001. In this paper, lowand high-resolution optical spectra obtained in 2000 May, June, and July are presented, which follow the spectral evolution from the early decline stage to the nebular stage.…”

Section: Introductionmentioning

confidence: 76%

“…We derive an amount of interstellar extinction E(B − V) = 0.92 ± 0.15 as an average of these results. Kiss et al (2001) also measured the equivalent widths of DIB, but their spectra contained only two of them at 5849 Å and 6613 Å. For this reason, their result has a large error E(B − V) = 0.85 ± 0.3.…”

Section: Interstellar Absorption Lines and Bandsmentioning

confidence: 99%

“…Kiss et al (2001) estimated the magnitude and the epoch of light maximum to have been m V 9 mag at 2000 May 5.0 UT, that is JD 2451669.5. Some slightly different parameters are proposed also, those are m V = 8.8 mag at JD 2451666 by Burlak & Esipov (2001) and m V = 9.2 mag at JD 2451671 by Lynch et al (2004).…”

Section: Introductionmentioning

confidence: 99%

“…Some slightly different parameters are proposed also, those are m V = 8.8 mag at JD 2451666 by Burlak & Esipov (2001) and m V = 9.2 mag at JD 2451671 by Lynch et al (2004). The parameters of Kiss et al (2001) are used in this paper. There are, however, some doubts about the epoch and the magnitude of light maximum, which are discussed in Sect.…”

Section: Introductionmentioning

confidence: 99%

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Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

Iijima¹

2012

A&A

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High-and low-resolution optical spectra of CI Aql were obtained during the outburst in 2000. Multiple absorption components of H I and Fe II lines were detected at the early decline stage. Their radial velocities were roughly −2500 km s −1 , −2200 km s −1 , −1700 km s −1 , and −1400 km s −1 , among which only the last components were likely still accelerating during the early decline stage. Prominent emission lines of [O III] and [N II] appeared about one month after light maximum. The duration of the nebular stage, however, was only one month and a few weeks. The ejected gas shells seem to have started to shrink about 70 days after light maximum. The amount of interstellar extinction is estimated to be E(B − V) = 0.92 ± 0.15 from the equivalent widths of the diffuse interstellar absorption bands. The helium abundance in the ejecta is estimated to be N(He) = 0.19 ± 0.05 and the mass of the ejecta to be about 2 × 10 −6 M . This object has been classified as a U Sco type recurrent nova, but its spectral evolution during the outburst resembled those of T Pyx type recurrent novae. It is doubtful whether the peak of m V 9 mag on 2000 May 5 was the true light maximum or an earlier brighter peak had been overlooked, because the spectral data suggest that the ejections of gas shells occurred prior to the discovery of the outburst on 2000 April 28.

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Section: Introductionmentioning

confidence: 76%

Section: Interstellar Absorption Lines and Bandsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

Iijima¹

2012

A&A

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“…High-velocity mass outflow is observed in recurrent novae (Anupama 2002;Iijima 2002;Kiss et al 2001;Anupama & Dewangan 2000;Lépine et al 1999;Munari et al 1999;Snijders 1987;Taylor et al 1989) and classical novae (Shore 2002;Iijima & Esenoglu 2003). In some of these objects as well as U Sco, nonspherical or jetlike mass ejections are suggested (Taylor et al 1989;Shore 2002).…”

Section: ϫ8mentioning

confidence: 99%

High-Velocity Jets in Recurrent Nova Outbursts

Kato

Hachisu

2003

The Astrophysical Journal

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Very fast bipolar mass outflows are suggested from emission-line profiles during the early stage of outbursts in the recurrent nova U Sco. The ejection velocity reaches 5000 or 6000 km s Ϫ1 at the optical peak and gradually decreases in time. Such properties have not been reproduced so far in nova theories. We propose a jet-shaped mass outflow as a mechanism of acceleration up to several thousand kilometers per second. The mass flow is accelerated where the jet is shaped, which is deep inside the region where the spherically symmetric winds would be accelerated. The terminal jet velocity depends sensitively on the white dwarf mass but weakly on other parameters.

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CI Aquilae :A recurrent nova with an unusually long plateau phase

Matsumoto

Ishioka

Uemura

et al. 2003

Monthly Notices of the Royal Astronomical Society

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We present the results of optical photometry of the recurrent nova CI Aql in a later phase of the outburst which occurred in 2000. Our observation revealed that the object reached the quiescent level between 2001 December and 2002 April, and therefore that CI Aql is a unique recurrent nova characterized by an extremely long (1.4–1.7 yr) plateau phase. The light curve obtained in the outburst suggests that the object is the first example of an intermediate between classical and recurrent novae. In comparison with the estimation given in published theoretical calculations, the long duration of the plateau phase supports a higher hydrogen content of the white dwarf envelope, whereas such an abundance of hydrogen requires a later cessation of the wind, which is in disagreement with the sudden fading observed in late November of 2000. The light curve obtained in the later phase of the outburst indicates that the object was fainter and the gradual decline was steeper than predicted. These discrepancies between the observation and the theoretical prediction demand a drastic modification of the present model of CI Aql.

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The 2000 outburst of the recurrent nova CI Aquilae: Optical spectroscopy

Cited by 31 publications

References 20 publications

Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

High-Velocity Jets in Recurrent Nova Outbursts

CI Aquilae :A recurrent nova with an unusually long plateau phase

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