Statistics – Computation
Scientific paper
Jul 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.233..405s&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 233, July 15, 1988, p. 405-422.
Statistics
Computation
4
Magnetohydrodynamic Flow, Neutron Stars, Particle Acceleration, Pulsar Magnetospheres, Computational Astrophysics, Current Density, Energy Dissipation, Stellar Magnetic Fields, Stellar Models
Scientific paper
A numerical simulation is performed for an axially symmetric and charge-separated magnetosphere of a neutron star with a circular flow which comes out from the neutron stars, suffers a strong relativistic acceleration causing the trans-field flow, and returns to the star. The location of the acceleration causing the trans-field flow is obtained as a function of the poloidal current density, and is found to be dependent on the magnetic field. It is shown that the magnetic field is determined by the convection current produced by the flow. The magnetic field structure is found to be closed. Relations between pulse period, pulse width, and poloidal current density are derived by means of the converged model and a marginal condition for the pair creation.
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