On the evolution of interacting, magnetized, galactic plasmas

Details On the evolution of interacting, magnetized, galactic plasmas On the evolution of interacting, magnetized, galactic plasmas

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..91...19p&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 91, no. 1, March 1983, p. 19-33. Research supported by the U.S. Department

Astronomy and Astrophysics

Astronomy

16

Computerized Simulation, Cosmic Plasma, Interstellar Magnetic Fields, Milky Way Galaxy, Plasma Interactions, Distribution Functions, Electron Acceleration, Electron Distribution, Electron Energy, Radio Sources (Astronomy), Relativistic Plasmas, Synchrotron Radiation, X Ray Sources

Scientific paper

The advent of three-dimensional, electromagnetic, and fully relativistic particle simulations allows a detailed study of a magnetized, rotating plasma, galaxy model. When two such models are simulated, an interaction yielding results resembling observational data from double radio sources, including the emission of synchrotron radiation, are obtained. Simulation-derived morphologies, radiation intensities, frequency spectra, and isophote patterns are directly compared to observations. The constituent plasma parameters associated with the source Cygnus A are found to be n(e) = 0.0018/cu cm, T = 2.8 keV, B = 20-30 gamma, with a small population of electrons accelerated to GeV energies by a rotation induced electric field. The results of these simulations, involving a computational resource of five CDC 7600 and five Cray-1 computers, strongly supports an inhomogeneous version of the Klein world model.

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