Hostname: page-component-6bf8c574d5-pdxrj Total loading time: 0 Render date: 2025-03-10T00:34:15.814Z Has data issue: false hasContentIssue false
  • English
  • Français

On the variations of [OIII] lines intensities in the spectrum of PN IC 4997

Published online by Cambridge University Press:  25 May 2016

A. G. Yeghikyan
A. G. Yeghikyan*
Affiliation:
Garni Space Astronomy Institute, Armenia

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The causes of asynchronous variations of the intensities of OIII ions forbidden lines in the spectrum of compact planetary nebula IC 4997 are considered on the basis of the observational data of. It is shown that the rise of the intensity of line 4363 å and decrease of the intensities of N 1 and N 2 lines may be best explained by increase of mass-loss-rate from nucleous from 5 × 10–8 up to 2 × 10–7 M/yr within a few years (at constant nucleous effective temperature), with appropriate change of ionization structure of nebula. The arguments of existence of variable hot stellar wind are discussed. The theoretical intensities of lines are calculated by the ionization model of planetary nebulae [4], gyven the radiation fields of the nucleous and hot stellar wind with electron temperature Te= 500000 K.

Type
IV. Envelopes
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 289
Copyright
Copyright © Kluwer 1997 

References

Hyung, S., et al., 1994, Astrophys. J. Suppl. Ser., 93, 465–483.Google Scholar
Kostyakova, E.B., 1991, Trans. Sternberg Astr. Inst., 62, 58–64.Google Scholar
Feibelman, W.A., 1982, Astrophys. J., 258, 562–566.Google Scholar
Egikyan, A.G., 1989, Astrofizika, 30, 270–281.Google Scholar
Adam, J. and Köppen, J., 1985, Astron. Astrophys., 142, 461–475.Google Scholar