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A three-dimensional magnetohydrodynamic model of planetary nebula jets, knots, and filaments - MaRDI portal

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A three-dimensional magnetohydrodynamic model of planetary nebula jets, knots, and filaments

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Publication:3614097

DOI10.1051/0004-6361:200809848zbMATH Open1156.85327arXiv0803.4518OpenAlexW2142596371WikidataQ68674563 ScholiaQ68674563MaRDI QIDQ3614097

Author name not available (Why is that?)

Publication date: 16 March 2009

Published in: (Search for Journal in Brave)

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.


Full work available at URL: https://arxiv.org/abs/0803.4518



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