  A good compromise between the resistive model and the PIC model is
Aristotelian electrodynamics, which can include the back-reaction of the
radiative photons onto particle motion and allow for a local dissipation where
the force-free condition is violated. We study the dissipative pulsar
magnetosphere with Aristotelian electrodynamics where particle acceleration is
fully balanced by radiation. The expression for the current density is defined
by introducing a pair multiplicity. The 3D structure of the pulsar
magnetosphere is then presented by solving the time-dependent Maxwell equations
using a pseudo-spectral algorithm. It is found that the dissipative
magnetosphere approaches the force-free solution and the dissipative region is
more restricted to the current sheet outside the light-cylinder (LC) as the
pair multiplicity increases. The spatial extension of the dissipative region is
self-consistently controlled by the pair multiplicity. Our simulations show the
high magnetospheric dissipation outside the LC for the low pair multiplicity.
