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A CO Search for Molecular Gas in High Mass Post-Main-Sequence Nebulae

Published online by Cambridge University Press:  12 April 2016

J.P. Phillips ,
A. Mampaso ,
N. Ukita  and
P.G. Williams
J.P. Phillips
Affiliation:
Instituto de Astrofisica de Canarias La Laguna, Tenerife, Spain
A. Mampaso
Affiliation:
Instituto de Astrofisica de Canarias La Laguna, Tenerife, Spain
N. Ukita
Affiliation:
Nobeyama Radio Observatory Tokyo Astronomical Observatory University of Tokyo, Japan
P.G. Williams
Affiliation:
Physics Department, Queen Mary College, London El 4NS, England

Extract

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High mass post-main-sequence nebulae are characterised by a set of unusual, and in certain cases extreme physical characteristics, including large outflow velocities (cf. Phillips and Mampaso, 1988a), extremely compact high emission measure cores (Phillips and Mampaso, 1988b), a high incidence of bipolar morphology (Peimbert and Torres Peimbert, 1982), and evidence for anomalously high levels of shock excited H2 S(l) emission towards both the source cores (Phillips et al 1983, 1985) and nebular peripheries (Zuckerman and Gatley, 1988). The large central star masses also predispose these sources to rapid evolution within the H-R plane (perhaps one or two orders of magnitude more rapid than for typical PN (Schonberner 1981, 1983), and the acquisition of stellar temperatures T* > 105 K, giving rise to correspondingly high levels of nebular excitation.

Type
III. Discs, Outflows, Jets and HH Objects
Information
International Astronomical Union Colloquium , Volume 120: Structure and Dynamics of the Interstellar Medium , 1989 , pp. 295 - 299
Copyright
Copyright © Springer-Verlag 1989

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