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arXiv · 0803.4518

A Three-Dimensional Magnetohydrodynamic Model of Planetary Nebula Jets, Knots, and Filaments

K. H. Tsui
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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 $M$. 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.

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K. H. Tsui. 2008-03-31. A Three-Dimensional Magnetohydrodynamic Model of Planetary Nebula Jets, Knots, and Filaments. https://doi.org/10.1051/0004-6361:200809848

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