From Bipolar to Elliptical: Morphological Changes in the Temporal Evolution of PN
Abstract
Proto-planetary nebulae (pPN) and planetary nebulae (PN) seem to be formed by interacting winds from asymptotic giant branch (AGB) stars. The observational issue that most pPN are bipolar but most older PN are elliptical is addressed. We present 2.5D hydrodynamical numerical simulations of episodic cooling interacting winds to investigate the long term evolution of PN morphologies. We track wind acceleration, decrease in mass-loss and episodic change in wind geometry from spherical (AGB) to collimated (pPN) and back to spherical again (PN). This outflow sequence is found to produce realistic PN dynamics and morphological histories. Effects from different AGB distributions and jet duty cycles are also investigated.
Keywords
Cite
@article{arxiv.1011.4312,
title = {From Bipolar to Elliptical: Morphological Changes in the Temporal Evolution of PN},
author = {Martin Huarte Espinosa and Adam Frank and Bruce Balick and Orsola De Marco and Joel H. Kastner and Raghvendra Sahai and Eric G. Blackman},
journal= {arXiv preprint arXiv:1011.4312},
year = {2010}
}
Comments
5 pages, 1 figure. To appear in the proceedings of the conference "Asymmetric Planetary Nebulae V", eds. Zijlstra, et al., editorial: Ebrary