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Family links between Planetary Nebulae nuclei and cataclysmic variables, binary white dwarfs, R CrB stars, and SNe IA

Published online by Cambridge University Press:  25 May 2016

L.R. Yungelson  and
A.V. Tutukov
L.R. Yungelson
Affiliation:
Astronomical Institute of the Russian Academy of Sciences 48 Pyatnitskaya Str., 109017 Moscow, Russia
A.V. Tutukov
Affiliation:
Astronomical Institute of the Russian Academy of Sciences 48 Pyatnitskaya Str., 109017 Moscow, Russia

Abstract

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We analyse the population of PNe and links between binary PNNi and stars which are in the later evolutionary stages. In a model which assumes that all stars are born in binaries, about 16% of PN result from ejection of common envelopes in close binaries, 85% of single PNNi are formed by merger of components of binaries. In the model, 5% of PNNi may be precataclysmic binaries, 5% may be precursors of symbiotic stars, 0.4% may be pre-SN Ia, 0.1% - precursors of hydrogen-deficient giants. About 0.1% of all PNe may be hydrogen-deficient.

Type
III. Central Stars
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 85 - 90
Copyright
Copyright © Kluwer 1997 

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