  The origins of the diffuse flux of cosmogenic PeV neutrinos detected in the
IceCube experiment during 2010 - 2017 remain unidentified. A population of
extragalactic newly born fast spinning pulsars are investigated as possible
candidates for generating the PeV energy scale neutrinos. A two-step mechanism
of particle acceleration is adopted for transferring energy from star rotation
to high energy electrons. Electrons might be boosted up to $\approx 0.01$ EeV
energies and above, and produce ultra-high-energy (UHE) neutrinos and gamma
rays when these electrons interact with low energy positrons and soft
radiations in the acceleration zone. The theoretically derived extragalactic
diffuse muon neutrino flux in the energy range [1-10] PeV is found consistent
with the IceCube level if only a fraction ($\eta_{k} \approx 0.31\%$) of the
total bolometric luminosity of pulsars are transferred to power the PeV
neutrinos. Using the above value of the cosmic ray electron loading parameter
$\eta_{k}$, the diffuse gamma ray flux from inverse Compton scattering off UHE
electrons in the soft radiation field might be predicted from the model.
