Abstract
Numerical models of the formation and propagation of magnetized extragalactic jets through flattened confining gas clouds where pressure and density fall off essentially as power laws are presented. These calculations follow the boundary between an ejected relativistic fluid and the shocked and swept-up galactic atmosphere. In these computations the magnetic effects are included by assuming that a fixed fraction of the total power is in the form of ordered magnetic fields. Earlier work showed that the collimation can be improved if the bulk of the azimuthal field component is external to the jet, presumably in a cocoon around the jet. Assuming this topology, it is found that good large-scale collimation can be obtained if reasonable magnetic energy densities and gas cloud parameters are chosen. However, if the fraction of the gross power devoted to magnetic fields exceeds 0.10-0.20, the jets quickly become unstable. 22 references.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
