  The magnetospheric plasma distribution in the vicinity of a pulsar at various
inclination angles is investigated using a new relativistic, parallel 3D
Particle-In-Cell (PIC) code DYMPHNA3D. DYMPHNA3D uses a superposition of the
electromagnetic fields associated with a rotating magnetised conducting sphere
in a vacuum (the pulsar fields) and the electromagnetic fields due to the
presence of the magnetospheric plasma surrounding the pulsar (the plasma
fields), as the total fields. The plasma is moved self-consistently through the
magnetosphere using the PIC methodology. Our initial simulation results are
presented here. These show similar solutions to those obtained from previous
numerical simulations, which show the fundamental plasma distribution in the
vicinity of an aligned rotating neutron star to consist of two polar domes and
an equatorial torus of trapped non-neutral plasma of opposite sign. The aligned
case being the case in which the inclination angle between the magnetic dipole
moment and the rotation axis of the star is zero. Furthermore, our code allows
for off-axis simulations and we have found that this plasma distribution
collapses into a Quad-Lobe charge-separated non-neutral magnetospheric plasma
distribution in the case of an orthogonal rotator, i.e., the case in which the
magnetic dipole moment is oriented at right angles to the rotation axis of the
neutron star, with the plasma remaining trapped close to the stellar surface by
the force-free surfaces. We find that if initialised with a Goldreich-Julian
type distribution, the system is seen to collapse rapidly into these stable
Dome-Torus structures.
