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Understanding the immediate progenitors of planetary nebulae

Published online by Cambridge University Press:  30 August 2012

R. Sahai ,
M. R. Morris ,
C. Sánchez Contreras  and
M. J. Claussen
R. Sahai
Affiliation:
Jet Propulsion Laboratory, Caltech, Pasadena, CA 91109, email: [email protected]
M. R. Morris
Affiliation:
Dept. of Phys. & Astr., UCLA, Los Angeles, CA 90095, email: [email protected]
C. Sánchez Contreras
Affiliation:
Astrobiology Center (CSIC-INTA), Madrid, Spain, email: [email protected]
M. J. Claussen
Affiliation:
NRAO, 1003 Lopezville Road, Socorro, NM 87801, email: [email protected]
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Abstract

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Pre-Planetary Nebulae (PPNe) are believed to represent a relatively short, intermediate evolutionary phase in the evolution of AGB stars to Planetary Nebulae (PNe). Our unbiased, high-resolution imaging surveys with HST of young PNe and PPNe show very strong morphological similarities between these classes, enabling us to extend our morphological scheme for PPN classification to young PNe, preserving virtually all of the primary and secondary descriptors, and adding a few new ones. These morphological surveys show that the primary shaping of PNe begins during the PPNe and/or late-AGB phase, and the key to understanding the shaping process lies in the study of these PNe progenitors. Here we present results from two recent studies of PNe progenitors: (i) Hα emission with very broad wings and P-Cygni profiles as probes of the region where the fast post-AGB outflows that do the shaping are most likely launched from, and (ii) equatorial waists with large-sized dust grains and large masses.

Keywords

Stars: AGB and post-AGBstars: mass-lossaccretion disksbinaries: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 180 - 183
Copyright
Copyright © International Astronomical Union 2012

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