  Pulsar magnetospheres have strong magnetic fields and large amounts of
plasma. The structures of these magnetospheres are studied using force-free
electrodynamics. To understand pulsar magnetospheres, discussions must include
their outer region. However, force-free electrodynamics is limited in it does
not handle dissipation. Therefore, a resistive pulsar magnetic field model is
needed. To break the ideal magnetohydrodynamic (MHD) condition $E \cdot B = 0$,
Ohm's law is used. In this work, I introduce resistivity depending upon the
distance from the star and obtain a self-consistent steady state by time
integration. Poloidal current circuits form in the magnetosphere while the
toroidal magnetic-field region expands beyond the light cylinder and the
Poynting flux radiation appears. High electric resistivity causes a large space
scale poloidal current circuit and the magnetosphere radiates a larger Poynting
flux than the linear increase outside of the light cylinder radius. The formed
poloidal current circuit has width, which grows with the electric conductivity.
This result contributes to a more concrete dissipative pulsar magnetosphere
model.
