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The Formation of Single and Binary Nuclei of Planetary Nebulae

Published online by Cambridge University Press:  07 August 2017

L. R. Yungelson  and
A. V. Tutukov
L. R. Yungelson
Affiliation:
Institute for Astronomy, 48 Pyatnitskaya Str., 109017 Moscow, Russia
A. V. Tutukov
Affiliation:
Institute for Astronomy, 48 Pyatnitskaya Str., 109017 Moscow, Russia

Extract

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The present birthrate of binaries may be written as

where M1 is the mass of the primary in M⊙, 0 < q ≤ 1 — mass ratio of components, A — semimajor axis of the orbit in R⊙. The Eq.(1) implies that all stars are born as binaries with 10 ≤ A/R⊙ ≤ 106, and that one binary with M1 ≥ 0.8M⊙ is formed annually in the Galaxy. We study numerically evolutionary scenarii of binaries within abovementioned range of M1, A,q. As PN formation events we consider all ejections of common envelopes by close binaries and ejections of envelopes by red giants, after which one may expect a formation of a hot (Te ≥ 30 000K) star, surrounded by a nebula. Altogether about 20 different single and binary cores of PN can be formed. Combining the scenarii data with the Eq. (1) one can estimate the birthrates of most numerous kinds of PNN (single and with main-sequence, white dwarf, giant and relativistic companions) listed in the Table.

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 389
Copyright
Copyright © Kluwer 1993