  We propose a simple explanation for the apparent dearth of radio pulsars
associated with young supernova remnants (SNRs). Recent X-ray observations of
young remnants have revealed slowly rotating (P ~ 10-s) central pulsars with
pulsed emission above 2 keV, lacking in detectable radio emission. Some of
these objects apparently have enormous magnetic fields, evolving in a manner
distinct from the Crab pulsar. We argue that these X-ray pulsars can account
for a substantial fraction of the long sought after neutron stars in SNRs and
that Crab-like pulsars are perhaps the rarer, but more highly visible example
of these stellar embers. Magnetic field decay likely accounts for their high
X-ray luminosity, which cannot be explained as rotational energy loss, as for
the Crab-like pulsars. We suggest that the natal magnetic field strength of
these objects control their subsequent evolution. There are currently almost a
dozen slow X-ray pulsars associated with young SNRs. Remarkably, these objects,
taken together, represent at least half of the confirmed pulsars in supernova
remnants. This being the case, these pulsars must be the progenitors of a vast
population of previously unrecognized neutron stars.
