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

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

2008-03-31

arxiv.org/abs/0803.4518v1

Astronomy and Astrophysics

Astrophysics

Scientific paper

10.1051/0004-6361:200809848

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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