The Transition to Axisymmetrical Mass Loss

Details The Transition to Axisymmetrical Mass Loss The Transition to Axisymmetrical Mass Loss

1999-09-15

arxiv.org/abs/astro-ph/9909258v1

Astronomy and Astrophysics

Astrophysics

6 pages, To appear in Asymmetrical Planetary Nebulae II, ASP Conference Series, J.H. Kastner, N. Soker, & S. Rappaport, eds

Scientific paper

Any model for the formation of elliptical planetary nebulae (PNs) should account for the positive correlation between the mass loss rate and the degree of departure from sphericity of the AGB progenitor's wind. I propose that this correlation results from dust formation above magnetic cool spots. The model deals with elliptical PNs, but not with bipolar PNs. The basic assumption is that a weak dynamo amplifies magnetic fields in AGB stars, such that magnetic cool spots are formed, mainly near the equatorial plane. Enhanced dust formation above these cool spots leads to a higher mass loss rate in the equatorial plane, resulting in the formation of an elliptical PN. The dust formation above cool spots becomes much more efficient when mass loss rate is high. In addition to explaining the correlation, the model has the advantage that it can operate for very slowly rotating AGB stars, having rotation velocities of less than $10^{-4}$ times the break-up velocity. Such velocities can be achieved by a planet companion of mass $\sim 0.1 M_{\rm Jupiter}$ which spins-up the envelope, or even from singly evolved stars which leave the main sequence with a high rotation velocity. The sporadic nature of magnetic cool spots also leads to the formation of filaments, arcs, and clumps in the descendant PN. The model cannot explain the presence of jets and ansae in elliptical PNs. These are attributed to the destruction of a planet or brown dwarf on the AGB core.

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