  We reconsider pulsar electrodynamics for an obliquely rotating pulsar, and
propose a way of synthesizing the vacuum dipole model (VDM) and the rotating
magnetosphere model (RMM). We first modify the VDM by assuming that the
parallel component of the inductive electric field is screened by charges. We
refer to the resulting model as the minimal model. We calculate the screening
charge density in the minimal model and compare it with the (Goldreich-Julian)
charge density in the RMM. We identify the plasma velocity in the minimal model
as the electric drift velocity due to the perpendicular component of the
inductive electric field. We define a class of synthesized models as a linear
combination of a fraction $y$ times the minimal model and $1-y$ times the RMM.
These models require a gap (with $E_\parallel\ne0$) between the corotating
stellar surface and the non-corotating magnetosphere. We present illustrative
plots of the charge density, of the location of nulls (where the charge density
is zero) and of the three components of the plasma velocity as a function of
the angles ($\theta,\psi$) relative to the rotation axis, for specific values
of the obliquity $\alpha$ and the parameter $y$. We discuss the question "Can
any pulsar magnetosphere be corotating?" critically, pointing out difficulties
associated with setting up corotation in the polar cap region. We speculate
that the corotating plasma may flow across the last closed field line from the
closed-field region. We suggest that abrupt changes in the spin-down rate in
some pulsars may be due to jumps between the RMM and the minimal model.
