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The stability of astrophysical jets

Published online by Cambridge University Press:  24 February 2011

Philip E. Hardee
Philip E. Hardee*
Affiliation:
Department of Physics & Astronomy, Gallalee Hall, The University of Alabama, Tuscaloosa, AL 35487USA email: phardee@bama.ua.edu
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Abstract

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Jets are produced by young stellar objects (YSOs), by black hole binary star system “microquasars” (μQSOs), by active galactic nuclei (AGN), are associated with neutron stars and pulsar wind nebulae (PWNe), and are thought responsible for the gamma-ray bursts (GRBs). An understanding of these outflows must include how they are launched and collimated into jets, and how they propagate to large distances. Jets be they Poynting flux and/or kinetic flux dominated are current driven (CD) and/or Kelvin-Helmholtz (KH) velocity shear driven unstable. Here I present some of the work that is leading to a better understanding of the properties required for the observed relative stability of astrophysical jets.

Keywords

Galaxies: jetsISM: jets and outflows(magnetohydrodynamics:) MHDinstabilitiesrelativity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 41 - 49
Copyright
Copyright © International Astronomical Union 2011

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