The Formation of Collimated Outflows and Concentric Rings in Magnetized Planetary Nebulae

Details The Formation of Collimated Outflows and Concentric Rings in Magnetized Planetary Nebulae The Formation of Collimated Outflows and Concentric Rings in Magnetized Planetary Nebulae

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002rmxac..12..127f&link_type=abstract

Ionized Gaseous Nebulae, a Conference to Celebrate the 60th Birthdays of Silvia Torres-Peimbert and Manuel Peimbert, Mexico City

Astronomy and Astrophysics

Astronomy

3

Hydrodynamics, Ism: Jets And Outflows, Ism: Bubbles, Planetary Nebulae: General, Stars: Agb

Scientific paper

Magnetic fields and wind asymmetries from rotating stars, along with precession of the stellar rotation axis, can create most of the observed Planetary Nebulae morphologies and collimated outflows (jets). The collimation of the flows by magnetic tension becomes very efficient after the magnetized wind has passed through the reverse shock of the PN. Also, the concentric rings observed in some PNe can be explained by a solar-like magnetic cycle with periodic polarity inversions.

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