Detailed optical behavior of the 2000 outburst of the eclipsing recurrent nova CI Aquilae

Matsumoto, Katsura; Uemura, Makoto; Katô, Takeo; Kiyota, S.; Ayani, K.; Kawabata, Tetsuya; Král, L.; Havlík, T.; Kolasa, M.; Novák, Rudolf

doi:10.1051/0004-6361:20011234

Cited by 18 publications

(32 citation statements)

References 22 publications

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“…The high-resolution spectra obtained on 2000 May 15 and 16 displayed nearly the same features. The high intensities of the emission lines of nitrogen ions were also reported in previous works (Burlak & Esipov 2001;Kiss et al 2001;Matsumoto et al 2001). …”

Section: Spectral Evolutionsupporting

confidence: 86%

“…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: 77%

“…They inferred that the object was in the post-maximum stage, because the spectrum contained prominent H I emission lines without any P Cygni type absorption component. Matsumoto et al (2001) carried out a detailed analysis for the same spectrum and found out the Fe II, He I, He II, N II, and N III emission lines, in addition to H I lines. This result supports the interpretation of Uemura & Kato (2000), because these lines, except for H I and Fe II, do not appear in the spectra of classical novae at the pre-maximum stage (McLaughlin 1960).…”

Section: Doubts About Light Maximum Of the Outburst In 2000mentioning

confidence: 99%

“…Matsumoto et al (2001) called attention to the work of Williams (2000), who estimated the maximum luminosity of the outburst in 1917 to have been 8.6 mag in the Tycho B band according the survey of Harvard College Observatory Patrol plates. The difference between the Tycho B band and the Johnson B band is not important in this argument.…”

Section: Doubts About Light Maximum Of the Outburst In 2000mentioning

confidence: 99%

“…Matsumoto et al (2001) and Lederle & Kimeswenger (2003) analysed the eclipsing light curve after the outburst in 2000. Lederle & Kimeswenger (2003) reported that the orbital period slightly lengthened after the outburst.…”

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: Spectral Evolutionsupporting

confidence: 86%

Section: Introductionmentioning

confidence: 77%

Section: Doubts About Light Maximum Of the Outburst In 2000mentioning

confidence: 99%

Section: Doubts About Light Maximum Of the Outburst In 2000mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Iijima¹

2012

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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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