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Morphology & Kinematics of the ‘Born–Again’ Planetary Abell 78

Published online by Cambridge University Press:  07 August 2017

R.E.S. Clegg ,
M.N. Devaney ,
A.P. Doel ,
C.N. Dunlop ,
J.V. Major ,
R.M. Myers  and
R.M. Sharples
R.E.S. Clegg
Affiliation:
Royal Greenwich Observatory, Madingley Rd, Cambridge CB3 0EZ, UK
M.N. Devaney
Affiliation:
Royal Greenwich Observatory, Madingley Rd, Cambridge CB3 0EZ, UK
A.P. Doel
Affiliation:
Physics Dept., University of Durham, Durham DH1 3LE, UK
C.N. Dunlop
Affiliation:
Physics Dept., University of Durham, Durham DH1 3LE, UK
J.V. Major
Affiliation:
Physics Dept., University of Durham, Durham DH1 3LE, UK
R.M. Myers
Affiliation:
Physics Dept., University of Durham, Durham DH1 3LE, UK
R.M. Sharples
Affiliation:
Physics Dept., University of Durham, Durham DH1 3LE, UK

Extract

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Abell 78 is one of a group of planetaries having an old, H–rich nebula surrounding a hot star which has more recently ejected highly–processed, H–deficient material. The A78 central star has O VI emission lines and a 3700 km s−1 hot wind, and is surrounded by knots of very dusty, H-deficient material. These objects are thought to have suffered a late helium shell flash which resulted in the central star (then a white dwarf) returning to the AGB and ejecting highly-processed material.

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 388
Copyright
Copyright © Kluwer 1993