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

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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Cited by in corpus (3)

• Non-detection of magnetic fields in the central stars of the planetary nebulae NGC 1360 and LSS 1362
• Magnetic fields in central stars of planetary nebulae?
• Homologous Gravitational Collapse in Lagrangian Coordinate: Planetary System in Protostar and Cavity in Pre-Supernova