  The current state of the art in the modeling of pulsar magnetospheres invokes
either the vacuum or force-free limits for the magnetospheric plasma. Neither
of these limits can simultaneously account for both the plasma currents and the
accelerating electric fields that are needed to explain the morphology and
spectra of high-energy emission from pulsars. To better understand the
structure of such magnetospheres, we combine accelerating fields and force-free
solutions by considering models of magnetospheres filled with resistive plasma.
We formulate Ohm's Law in the minimal velocity fluid frame and construct a
family of resistive solutions that smoothly bridges the gap between the vacuum
and the force-free magnetosphere solutions. The spin-down luminosity, open
field line potential drop, and the fraction of open field lines all transition
between the vacuum and force-free values as the plasma conductivity varies from
zero to infinity. For fixed inclination angle, we find that the spin-down
luminosity depends linearly on the open field line potential drop. We consider
the implications of our resistive solutions for the spin down of intermittent
pulsars and sub-pulse drift phenomena in radio pulsars.
