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OH Maser Emission from Young Planetary Nebulae

Published online by Cambridge University Press:  19 July 2016

A. Zijlstra ,
S. R. Pottasch ,
P. te Lintel  and
C. Bignell
A. Zijlstra
Affiliation:
NRAO/VLA
S. R. Pottasch
Affiliation:
Kaypteyn Institute, Groningen
P. te Lintel
Affiliation:
Kaypteyn Institute, Groningen
C. Bignell
Affiliation:
NRAO/VLA

Abstract

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OH/IR stars are now generally accepted to be progenitors of planetary nebulae. We have carried out a project to try to find objects in the transition phase between OH/IR stars and PN. Transition objects should be characterized by having both continuum radio emission and a 1612 MHz OH maser line. The continuuum emission would indicate that the central star has become hot enough to ionize part of the envelope, while the OH maser indicates that a large part of the envelope is still neutral. Only one such object was known, namely Vy 2-2.

Type
II. Nebular Properties
Information
Symposium - International Astronomical Union , Volume 131: Planetary Nebulae , 1989 , pp. 210
Copyright
Copyright © Kluwer 1989