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Mass Loss from Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  18 September 2017

M. Perinotto
M. Perinotto*
Affiliation:
Osservatorio Astrofisico di Arcetri, Firenze, Italy

Abstract

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Stellar winds have been revealed in a large fraction of central stars of planetary nebulae from P Cygni profiles observed with the IUE satellite. The relevant lines are essentially the resonance lines NV λ 1240, Si IV λ 1397, CIV λ 1549 and the subordinate lines OIV∗ λ 1342, 0V∗ λ 1371, NIV∗ λ 1579. Edge velocities are of the order of 1000-3000 km s−1, similar to the case of population I O stars. Detailed determinations of the mass loss rate have been performed for NGC 6543, NGC 2371, IC 2149 and IC 3568 with values between 4.10−9 to 7. 10−7 Mo yr−1. The accuracy of these determinations is not well known. It is however clear from the variety of observed profiles in these and in several other objects that properties of the winds (ionization structure, etc.) varies considerably from object to object and that very likely the mass loss rate will span over a large interval. Some possible consequences of these winds are discussed.

Type
Section IV: Origin of Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 103: Planetary Nebulae , 1983 , pp. 323 - 335
Copyright
Copyright © Reidel 1983 

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