Radio Pulsar Emission from Closed and Filled Magnetospheric Shells

Details Radio Pulsar Emission from Closed and Filled Magnetospheric Shells Radio Pulsar Emission from Closed and Filled Magnetospheric Shells

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...464..359m&link_type=abstract

Astrophysical Journal v.464, p.359

Astronomy and Astrophysics

Astronomy

2

Magnetohydrodynamics: Mhd, Stars: Pulsars: General, Radiation Mechanisms: Nonthermal

Scientific paper

Curvature radiation from particles streaming along magnetic field lines on the closed surface of revolution generated by a single field line is considered to be a major source of time-averaged, radio pulsar emission. Emission from each field line is assumed to be the product of classical, single-particle emission, Pm, and a coherence coefficient, Cm, the latter depending only on the number of electrons, N, phase bunched over an angle, ψ, on any field line of the shell. Integration over all field lines on the surface then gives the postulated emission. Such a model produces pulses that replicate the time evolution of the peak-to-peak separation, fine structure, and frequency dependence of two pulsars with distinctly different morphologies.

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