  Charged particles can be accelerated to higher than PeV energies in the
electro-magnetic wind of a fast-spinning newborn pulsar to produce high-energy
neutrinos, through hadronuclear interactions in the supernova remnant. Here we
explore the detectability and observational signatures of these high-energy
neutrinos. We show that their spectral index varies approximately from 1.5 to
2, depending on the relevant pulsar properties and observation time. We also
apply the scenario to existing young pulsars in the local universe and find the
corresponding neutrino flux well below current detection limits. Finally, we
estimate the birth rate of fast-spinning pulsars in the local Universe that can
be observed by the IceCube observatory to be 0.07 per year, with an upper limit
of 0.29 per year.
