Flow Dynamics in Pulsar Magnetosphere Models with Particle Inertia

Abstract

Steadily rotating neutron star magnetospheres, with the Lorentz force balanced by inertia, are studied. It is assumed that charged particles leave the star with nonrelativistic speeds and that any returning are decelerated so as to be nonrelativistic on impact. No assumptions are made as to where in the magnetosphere substantial acceleration occurs or as to the degree of charge separation. It is found that the main qualitative features of the flow dynamics for the general oblique rotator can be understood by regarding the poloidal speed Vp as a parameter for the azimuthal speed v and Lorentz factor y of a species, and then considering flow curves that represent the variation of v;/c2 along each poloidal streamline. There are two possible flow branches--solutions for v and y-for each curve. One is applicable where the dimensionless non-corotational electric potential

1 -1/x2 there, but is never valid where

1. The flow branches can meet, with infinite gradients of v and y, corresponding to failure of the dissipation-free flow.