Stagnation Knots in Planetary Nebulae

Details Stagnation Knots in Planetary Nebulae Stagnation Knots in Planetary Nebulae

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002rmxac..12..152s&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

1

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

Scientific paper

We present an alternative model for the formation of fast low-ionization emission regions (FLIERs) in planetary nebulae. In this model, a concave bow-shock structure is formed as a result of a reduced momentum flow along the symmetry axis of a stellar wind. FLIERS are formed from the shocked ambient medium. Since in the concave region of the bow-shock the ambient material can not flow away from the symmetry axis, it is compressed into a dense knot or jet-like feature. In the presence of a variable stellar wind these knots eventually overrun the expanding nebular shell and may appear as detached FLIERS. We present two-dimensional hydrodynamic simulations of the formation and early evolution of stagnation knots and jets.

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