Molecular lines from protoplanetary nebulae: observations with ALMA
Planetary nebulae (PNe) are formed in a very fast process. In just about 1000 years, the nebula evolves from a spherical and slowly expanding AGB envelope to a PN, with usually axial symmetry and high axial velocities. Molecular lines are known to probe most of the nebular material in young PNe and protoplanetary nebulae (PPNe), and are therefore very useful to study such an impressive evolution. Many quantitative results on these objects have been so obtained, including general structure, total mass and density distribution, kinetic temperatures, velocity fields, etc. Existing observations probe both the gas accelerated by post-AGB shocks and the quiescent components. But the study of crucial regions to understand PN formation (recently shocked shells, regions heated by the stellar UV and inner rotating disks) requires observations at higher frequency and with better spatial resolution.
Keywords(Stars:) circumstellar matter Stars: AGB and post-AGB Stars: mass loss Radio lines: stars
PACS97.10.Fy 97.10.Me 98.38.Ly 98.58.Li
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- Alcolea, J., Neri, R., Bujarrabal, V.: Astron. Astrophys., in press (2007) Google Scholar
- Bujarrabal, V.: In: Barlow, M.J., Méndez, R.H. (eds.) IAU Symp. No 234, Planetary Nebulae in our Galaxy and Beyond, p. 193. Cambridge University Press, Cambridge (2006) Google Scholar
- Bujarrabal, V., van Winckel, H., Neri, R., et al.: Astron. Astrophys., in press (2007) Google Scholar
- Fong, D., Meixner, M., Castro-Carrizo, A., et al.: Astrophys. J. 367, 652 (2001) Google Scholar