Three-dimensional magnetic field configurations in relativistic magnetohydrodynamic outflows

Details Three-dimensional magnetic field configurations in relativistic magnetohydrodynamic outflows Three-dimensional magnetic field configurations in relativistic magnetohydrodynamic outflows

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...397l..67l&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 397, no. 1, p. L67-L70.

Astronomy and Astrophysics

Astronomy

10

Magnetic Field Configurations, Magnetohydrodynamic Flow, Radio Jets (Astronomy), Relativistic Plasmas, Supernova Remnants, Three Dimensional Models, Extragalactic Radio Sources, Perturbation Theory, Pulsars, Stellar Winds, Synchrotron Radiation

Scientific paper

A class of steady 3D relativistic magnetohydrodynamic (RMHD) winds is constructed from a primary radial RMHD outflow of spherical symmetry. The energetic source for modifying the given radial wind is the Poynting flux into the outflowing plasma due to interaction of transverse flow and magnetic field at a reference sphere surrounding a central object. The energy flux associated with such three-dimensional transverse RMHD perturbations is conserved to the leading order of large radial distance r. Asymptotically, the radial magnetic field B0 varies as 1/r-squared while transverse field b approaches about 1/r such that b dominates B0 at large r. Furthermore, the nonlinear effect of transverse electric force due to charge separation acts against transverse magnetic force. Since magnetic field configurations and their strengths are crucial for a realistic modeling of synchrotron emissions, the class of three-dimensional RMHD winds described here provides an important basis for synchrotron calculations which can be used to probe the structures of extragalactic radio jets and supernova remnants.

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