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Formation of bipolar planetary nebula M 2-9 by confining toroidal magnetic field and surrounding high-ram pressure wind

Published online by Cambridge University Press:  15 December 2006

Haruichi Washimi ,
Gary P. Zank ,
Takashi Tanaka  and
Bruce Balick
Haruichi Washimi
Affiliation:
Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521, USA email: washimih@ucr.edu
Gary P. Zank
Affiliation:
Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521, USA email: washimih@ucr.edu
Takashi Tanaka
Affiliation:
Faculty of Science, Kyushu University, Hakozaki, Fukuoka 812-8581, Japan
Bruce Balick
Affiliation:
Department of Astronomy, University of Washington, Seattle, Washington 98195, USA
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Abstract

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We model the highly axisymmetric planetary nebula M2-9 using a global 3-D MHD simulation. We assume that there is no high-density circumstellar gas around M2-9, because termination shocks are missing at the top of the bipolar lobes in optical images. The overall structure of our MHD solution is a self-consistent consequence of the stellar wind itself, corresponding to two kinds of circumstellar gas distributions, one a collimated flow and the other enveloping the collimated flow. Thus our model shows a ‘solitary stellar wind’ forming in a diluted circumstellar gas density.

Keywords

Planetary nebulae: individual (M2-9)MHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 543 - 544
Copyright
© 2006 International Astronomical Union