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Mass Loss Rates in Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  19 July 2016

M. Perinotto
M. Perinotto*
Affiliation:
Istituto di Astronomia, Università di Firenze, Italy

Abstract

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Central stars of planetary nebulae (PNCS) frequently exhibit fast winds (cf. Cerruti-Sola and Perinotto, 1985; C.P. and Grewing, this volume). They may be important for the structure of the whole nebula as well as for the evolution of the central star. Their speed is typically two orders of magnitude higher than that of the classical optically visible nebula, which in turn expands a few times faster than the most external winds detected in few cases in the radio domain.

I review here the status of art in the determination of the mass loss rates (M) associated with these fast winds. I restrict myself to the ‘observational’ determinations. Only at the end I will say something about the predictions of multi-scattering line radiation wind driven theory in connection with one best studied object: N6C 6543. This allows one to conclude that this theory may be the right explanation also for these winds.

Type
III. Central Stars
Information
Symposium - International Astronomical Union , Volume 131: Planetary Nebulae , 1989 , pp. 293 - 300
Copyright
Copyright © Kluwer 1989 

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