Wave propagation in pulsar magnetospheres - Refraction of rays in the open flux zone

Details Wave propagation in pulsar magnetospheres - Refraction of rays in the open flux zone Wave propagation in pulsar magnetospheres - Refraction of rays in the open flux zone

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...302..138b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 302, March 1, 1986, p. 138-162. Research supported by the University of Cal

Statistics

Computation

118

Computational Astrophysics, Electron Plasma, Magnetic Flux, Pulsar Magnetospheres, Pulsars, Refracted Waves, Wave Propagation, Electron-Positron Plasmas, Hamiltonian Functions, Lorentz Force, Magnetohydrodynamic Waves, Polarization (Waves), Radio Emission

Scientific paper

The propagation of waves through a relativistically outflowing electron-positron plasma in a very strong dipolar magnetic field, conditions expected in pulsar magnetospheres, is investigated. Halmilton's equations is derived for the propagation of rays through a plasma which is inhomogeneous in density, magnetic field directions, and Lorentz factor. These equations are solved for rays propagating through the plasmas outflowing along the 'open' dipolar field lines in which the density decreases inversely as the radius cubed and in the case where gradients transverse to the radial direction exist. In the radial case, the effects of refraction on pulse profiles, spectrum, and polarization are examined, and the effects of a transverse gradient are indicated. Attention is given to models in which the observed broad bandwidth in the radio emission has its origin in a radius to frequency map. Models with broad-band emission at a single radius are also studied. These are compared to observations of pulse width and pulse component separation as a function of frequency. The origin of 'orthogonal modes' is discussed.

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