A Three-Dimensional Magnetohydrodynamic Model of Planetary Nebula Jets, Knots, and Filaments
Astrophysics
2012-10-18 v1
Abstract
The morphologies of planetary nebulae are believed to be self-organized configurations. These configurations are modeled by three-dimensional temporally self-similar magnetohydrodynamic solutions with radial flow, under the gravitational field of a central star of mass . These solutions reproduce basic features, such as jets, point-symmetric knots, and filaments, through plasma pressure, mass density, and magnetic field lines. The time evolution function of the radial velocity starts as a slow wind and terminates as a fast wind.
Keywords
Cite
@article{arxiv.0803.4518,
title = {A Three-Dimensional Magnetohydrodynamic Model of Planetary Nebula Jets, Knots, and Filaments},
author = {K. H. Tsui},
journal= {arXiv preprint arXiv:0803.4518},
year = {2012}
}