Statistics – Computation
Scientific paper
Oct 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...237..329s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 237, no. 2, Oct. 1990, p. 329-335. Research supported by Villanova University.
Statistics
Computation
Astronomical Models, Computational Astrophysics, Extragalactic Radio Sources, Magnetic Field Configurations, Plasma Diffusion, Radio Jets (Astronomy), Incompressible Fluids, Interstellar Magnetic Fields, Rotating Fluids
Scientific paper
The diffusion of poloidal magnetic field in extragalactic radio sources is discussed. The development of an azimuthal field component is analyzed using different models for the rotation of the incompressible inviscid fluid and structures for the initial poloidal field component. It is shown that in some cases the generated azimuthal field achieves its maximum strength somewhere inside, close to the boundary of the jet proper. The region between the location where the azimuthal field gains its maximum strength and the boundary of the jet, or in some models the region of low-intensity reversed field surrounding the inner part, is then interpreted as the cocoon surrounding the jet which acts as a buffer zone against instabilities along the boundary of the jet.
No associations
LandOfFree
Models for diffusion of poloidal fields in extragalactic radio jets does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Models for diffusion of poloidal fields in extragalactic radio jets, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Models for diffusion of poloidal fields in extragalactic radio jets will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1301169