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On the Origin of Bipolar Planetary Nebulae

Published online by Cambridge University Press:  15 December 2006

Shigeki Miyaji  and
Daigo Saito
Shigeki Miyaji
Affiliation:
Department of Physics, Graduate school of Science and Technology, Chiba University, Chiba 2638522, Japan email: miyaji@astro.s.chiba-u.ac.jp
Daigo Saito
Affiliation:
Department of Physics, Graduate school of Science and Technology, Chiba University, Chiba 2638522, Japan email: miyaji@astro.s.chiba-u.ac.jp
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Abstract

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We present a numerical simulation of the formation of a bipolar planetary nebula from a single star. At the late stage of AGB stars, surface convection and/or convection of shell burning would create differential rotation between the core and the envelope of such stars. If the core has a magnetic field threading the envelope, this differential rotation twists magnetic fields. Then like a cosmic jet model of accretion disks, such a twist of magnetic fields piles up a tower of magnetic fields atop the pole of the progenitor core and creates jets.

Keywords

convectioninstabilitiesMHDplasmaplanetary nebulae: generalstars: post-AGB
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 551 - 552
Copyright
© 2006 International Astronomical Union