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Pulsar wind nebulae (PWNe) are outstanding accelerators in Nature, in thesense that they accelerate electrons up to the radiation reaction limit.Motivated by this observation, this paper examines the possibility that youngpulsar wind nebulae can accelerate ions to ultra-high energies at thetermination shock of the pulsar wind. We consider here powerful PWNe, fed bypulsars born with $\sim\,$millisecond periods. Assuming that such pulsarsexist, at least during a few years after the birth of the neutron star, andthat they inject ions into the wind, we find that protons could be acceleratedup to energies of the order of the Greisen-Zatsepin-Kuzmin cut-off, for afiducial rotation period $P\,\sim\,1\,$msec and a pulsar magnetic field$B_{\star}\,\sim\,10^{13}\,$G, implying a fiducial wind luminosity $L_{\rmp}\,\sim\,10^{45}\,$erg/s and a spin-down time $t_{\rm sd}\,\sim 3\times10^7\,$s. The main limiting factor is set by synchrotron losses in the nebulaand by the size of the termination shock; ions with $Z\geq 1$ may therefore beaccelerated to even higher energies. We derive an associated neutrino fluxproduced by interactions in the source region. For a proton-dominatedcomposition, our maximum flux lies slightly below the 5-year sensitivity ofIceCube-86 and above the 3-year sensitivity of the projected Askaryan RadioArray. It might thus become detectable in the next decade, depending on theexact level of contribution of these millisecond pulsar wind nebulae to theultra-high energy cosmic ray flux.

On ultra-high energy cosmic ray acceleration at the termination shock of young pulsar winds