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Properties which cannot be explained by Planetary Nebulae's progenitors

Published online by Cambridge University Press:  25 May 2016

Noam Soker*
Affiliation:
University of Haifa at Oranim

Extract

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Stellar binary companions account for bipolar PNe (∼ 11% of all PNe1), and some ellipticalls (22%2). The rest of axisymmetrical PNe (40% to 60% of all PNe) are due to substellar objects (planets and brown dwarfs)3. This classification of axi symmetrical PNe suggests that substellar objects are commonly present within several × AU around main sequence stars, and that several substellar objects must be present around most main sequence stars3. Some substellar and low mass stellar companions will enter the primary envelope only as the primary reaches the upper AGB. Thus, the early mass loss episode will be spherical, leading to the formation of a spherical halo around an elliptical inner region. Gas giant planets and brown dwarfs close to the primary, will not allow Earth-like planets to have stable orbits. Systems with no Jupiter-like planets will allow Earth-like planets to be present. These stars will form spherical PNe (10%-20% of all PNe, including spherically ejected PNe that have been deformed by the ISM through which they move4). Systems with substellar objects at large separation, as Jupiter in the solar system, will also allow Earth-like planets to be present. These systems will form PNe with spherical halo. Therefore, life may have been present in planets around the central stars of round PNe and elliptical PNe with round halos.

Type
V. From AGB to Planetary Nebulae
Copyright
Copyright © Kluwer 1997 

References

Schwarz, H. E., & Corradi, R. L. M. 1995, Asymmetrical Planetary Nebulae, eds. Harpaz, A. and Soker, N., p. 113.Google Scholar
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Soker, N. 1997, preprint.Google Scholar