Hostname: page-component-77c89778f8-5wvtr Total loading time: 0 Render date: 2024-07-19T12:14:39.191Z Has data issue: false hasContentIssue false
  • English
  • Français

How unique is the protoplanetary nebula star HR 4049?(*)

Published online by Cambridge University Press:  04 August 2017

C.L. Waelkens  and
L.B.F.M. Waters
C.L. Waelkens
Affiliation:
(1) Research Associate of the Belgian National Science Foundation, University of Leuven, Belgium
L.B.F.M. Waters
Affiliation:
(2) Space Research Laboratory, Utrecht, The Netherlands

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 late B-supergiant HR 4049 is peculiar in different respects: (1) It is located far from the galactic plane (b = 23°); (2) It is a variable with a large amplitude and on a long time scale (Waelkens and Rufener, 1983); (3) It has a spectacular infrared excess (Lamers et al., 1986). Two models were proposed: (i) HR 4049 is a runaway hypergiant embedded in a dust cloud, or (ii) HR 4049 is a low-mass star in a post-AGB stage of evolution. In this paper we present evidence that favours the second hypothesis. This evidence consists of new observational data on HR 4049 itself and of the discovery of a second very similar object, that is located still farther from the galactic plane.

Type
Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 122: Circumstellar Matter , 1987 , pp. 509 - 510
Copyright
Copyright © Reidel 1987 

References

Lamers, H.J.G.L.M., et al. (1986), Astron. Astrophys. 154, L20–L22.Google Scholar
Luck, R.E., Bond, H.E. (1984), Astrophys. J. 279, 729–737.Google Scholar
Waelkens, C., Rufener, F. (1983), Hvar Obs. Bull. vol. 7, no.1, p. 29.Google Scholar