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Hydrodynamics of ring nebulae: magnetic vs. non-magnetic hydro-models

Published online by Cambridge University Press:  25 May 2016

Guillermo García-Segura ,
Norbert Langer ,
Michał Różyczka ,
José Franco  and
Mordecai-Mark Mac Low
Guillermo García-Segura
Affiliation:
Instituto de Astronomía-UNAM, Apdo Postal 877, Ensenada, 22800 Baja California, Mexico
Norbert Langer
Affiliation:
Institut für Physik, Universität Potsdam, D-14415 Potsdam, Germany
Michał Różyczka
Affiliation:
N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warszawa, Poland
José Franco
Affiliation:
Institute de Astronomía-UNAM, Apdo Postal 70–264, 04510 México D.F., Mexico
Mordecai-Mark Mac Low
Affiliation:
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany

Abstract

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The formation of ring nebulae and their shapes is studied by numerical simulations. The old problem of the origin of the nebular shape is addressed. Two proposed mechanisms are discussed: stellar rotation and stellar magnetic fields, or a combination of both. Two and three-dimensional hydrodynamical and magneto-hydrodynamical simulations indicate that these processes are equally efficient in driving elliptical nebulae such as those surrounding Wolf-Rayet stars, like NGC 6888 around WR136. However, bipolar nebulae are better reproduced by rotation.

Type
Part 3. Interaction of Wolf-Rayet stars and other hot massive stars with their environment: colliding winds and ring nebulae
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 325 - 333
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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