FLIERs as stagnation knots from partially collimated outflows

Simple item page
dc.creatorSteffen, Wolfgang
dc.creatorLopez, Jose Alberto
dc.date1999-09-15
dc.date.accessioned2026-07-07T02:33:17Z
dc.date.available2026-07-07T02:33:17Z
dc.descriptionWe propose a new model for the formation of fast, low-ionization emission regions (FLIERs) in planetary nebulae that is able to account for many of their attendant characteristics and circumvent the problems on the collimation/formation mechanisms found in previous studies. In this model, FLIERs are formed in the stagnation zone of partially collimated stellar winds with reduced momentum flow along the axis. A concave bow-shock structure is formed due to the lack of momentum flow along the axis of a midly bipolar stellar wind. The stagnation knots are formed when the shocked environment medium accumulates at the apex of the outer shell and is compressed to a dense knot in the {\em concave} section of the bow-shock. We present two-dimensional hydrodynamic simulations of the formation of a stagnation knot and compare the resultant dynamical properties with those of FLIERs in planetary nebulae.
dc.description4 pages incl. 1 fig., to be published in the proceedings of the conference on Asymmetrical Planetary Nebulae II, PASP Conference Series, 2000, J.H. Kastner, N. Soker, S. Rappaport, eds
dc.identifierhttps://arxiv.org/abs/astro-ph/9909261
dc.identifierhttp://arxiv.org/abs/astro-ph/9909261
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/14784
dc.subjectAstrophysics
dc.titleFLIERs as stagnation knots from partially collimated outflows
dc.typetext

Files

Collections

arXiv