Hostname: page-component-78c5997874-mlc7c Total loading time: 0 Render date: 2024-11-14T18:15:13.968Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectrophotometry and Multicolour Imagery of the Planetary Nebula Around the P Cygni Star AG Carinae

Published online by Cambridge University Press:  07 August 2017

C. Rossi ,
A. Altamore ,
R.D.D. Costa ,
A. Damineli Neto ,
J.A. De Freitas Pacheco ,
A. Cassatella ,
A.R. Marenzi ,
P. Persi ,
V.F. Polcaro  and
R. Viotti
C. Rossi
Affiliation:
Ist. Astronomico, Univ. La Sapienza, Via Lancisi 29, 00161 Roma, Italy
A. Altamore
Affiliation:
Ist. Astronomico, Univ. La Sapienza, Via Lancisi 29, 00161 Roma, Italy
R.D.D. Costa
Affiliation:
Inst. Astron. e Geofís., Caixa Postal 9638, 01065 SÃo Paulo SP, Brasil
A. Damineli Neto
Affiliation:
Inst. Astron. e Geofís., Caixa Postal 9638, 01065 SÃo Paulo SP, Brasil
J.A. De Freitas Pacheco
Affiliation:
Inst. Astron. e Geofís., Caixa Postal 9638, 01065 SÃo Paulo SP, Brasil
A. Cassatella
Affiliation:
Ist. Astrofisica Spaziale, CNR, Via Fermi 21, 00044 Frascati RM, Italy
A.R. Marenzi
Affiliation:
Ist. Astrofisica Spaziale, CNR, Via Fermi 21, 00044 Frascati RM, Italy
P. Persi
Affiliation:
Ist. Astrofisica Spaziale, CNR, Via Fermi 21, 00044 Frascati RM, Italy
V.F. Polcaro
Affiliation:
Ist. Astrofisica Spaziale, CNR, Via Fermi 21, 00044 Frascati RM, Italy
R. Viotti
Affiliation:
Ist. Astrofisica Spaziale, CNR, Via Fermi 21, 00044 Frascati RM, Italy

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.

Some of the high luminosity stars in our Galaxy are surrounded by planetary-like nebulae formed by material ejected from the central star. The most interesting case is that of the ring nebula PK 289-0° 1 around the P Cygni star AG Car. Long slit spectroscopy shows that nitrogen is overabundant and oxygen underabundant in the nebula. The Hα/[NII] ratio is lower in the nebula with respect to the surrounding H II region, possibly as a result of the N overabundance in the stellar wind. The emission line peak separation confirms a model of a distorted spherical shell expanding at 66 km s−1. The scattered star's spectrum is observable near the star, suggesting the presence of circumstellar dust grains. A nebular mass of at least 2.7 M⊙ is derived. While the nebula in the Hα imagery reveals the ring-like shape with many structures, in the blue it is much fainter and smoother. No nebular emission was detected in the JHK bands, suggesting a low dust temperature.

Type
III. Highlights on the Nebulae
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 217
Copyright
Copyright © Kluwer 1993