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MHD Models of Planetary Nebulae: Review

Published online by Cambridge University Press:  26 May 2016

Guillermo García-Segura
Guillermo García-Segura*
Affiliation:
Instituto de Astronomía-UNAM, Apdo Postal 877, Ensenada, 22800 Baja California, Mexico

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When we discuss about MHD effects in planetary nebulae (PNe), there naturally arises a basic question: which magnetic field do we study? One possibility is the ISM magnetic field (e.g. Heiligman 1980), even more if we are concerned with moving PNe (e.g. Soker & Dgani 1997). The next possibility is the internal or stellar magnetic field (Gurzadian 1962). It is important to start this review by quoting Aller (1958): “It has been pointed out by Minkowski and others that the structural appearance of many planetary nebulae strongly suggest the presence of magnetic fields. It seems unlikely that such magnetic fields are produced ab initio in the nebular shell. Rather, they must have existed in the outer envelope of the parent star. Certain red giants stars with magnetic fields may evolve in such a way that the expansion of the shell is largely governed by the presence of such a field. Magnetic effects may actually be more important than gas pressure differentials and radiation pressure in controlling the evolution of a planetary nebula”.

Type
Part VII: Nebular Morphology and Dynamics
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 457 - 464
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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