Spectroscopic and photometric observations of the recurrent nova IM Normae

Duerbeck, H. W.; Sterken, C.; Baptista, R.; Diaz, M. P.; Dutra, Carlos Maximiliano; Freyhammer, L. M.; Hensberge, H.; Jones, A. F.

doi:10.1063/1.1518218

Cited by 2 publications

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“…It seems that T Pyx, IM Nor, and CI Aql form a sub-group of recurrent novae. This classification has been suggested also in some previous works (Anupama 2002;Duerbeck et al 2002;Kato et al 2002).…”

Section: Classification Of CI Aqlmentioning

confidence: 84%

“…The spectral evolution of CI Aql during the outburst in 2000, however, resembled those of T Pyx type recurrent novae. The spectral evolution of T Pyx in the outburst in 1966 was reported by Catchpole (1969), and that of IM Nor in 2002 was studied by Duerbeck et al (2002) and Liller (2002). The spectra of CI Aql at the early decline stage (Figs.…”

Section: Classification Of CI Aqlmentioning

confidence: 99%

“…Therefore, the forbidden lines appeared in the spectrum of U Sco at a much later stage of its evolution with respect to those of T Pyx, IM Nor, and CI Aql. Kato et al (2002) and Duerbeck et al (2002) pointed out that the light curves of T Pyx, IM Nor, and CI Aql resembled those of medium-fast classical novae. Their light curves, therefore, are different from those of U Sco (Rosino & Iijima 1988;Sekiguchi et al 1988), V394 CrA (Sekiguchi et al 1989), and Nova LMC 1990-2 (Sekiguchi et al 1990), which were characterised by the extremely fast fading.…”

Section: Classification Of CI Aqlmentioning

confidence: 99%

“…The three objects T Pyx, IM Nor, and CI Aql showed the prominent [O III] and [N II] lines in the outbursts: T Pyx (Catchpole 1969), IM Nor (Duerbeck et al 2002;Liller 2002), and CI Aql (Burlak & Esipov 2001;this paper). In contrast, no forbidden line was detected in the outbursts of U Sco type recurrent novae until Diaz et al (2010) (Rosino & Iijima 1988;Sekiguchi et al 1988;Munari et al 1999;Iijima 2002), V394 CrA (Sekiguchi et al 1989), and Nova LMC 1990-2 (Sekiguchi et al 1990).…”

Section: Classification Of CI Aqlmentioning

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: Classification Of CI Aqlmentioning

confidence: 84%

Section: Classification Of CI Aqlmentioning

confidence: 99%