  We calculate the flux of neutrinos generated by the propagation of ultra-high
energy nuclei over cosmological distances. The propagation takes into account
the interactions with cosmic background radiations including the CMB and the
most recent estimates of higher energy (infra-red, optical, and ultra violet)
backgrounds. We assume that the composition of ultra-high energy cosmic rays
(UHECRs) at the source is the same as the observed one at low energies. This
assumption fits well the present data at the highest energies. We compare the
cosmogenic neutrino flux from mixed composition sources to pure proton sources.
We find that the neutrino flux in the mixed composition case has a high energy
peak, mainly due to photopion production off CMB photons, of similar shape and
amplitude to the proton case. At low energies both composition cases have
significant neutrino flux with a peak around 1014.5 eV due to the higher energy
backgrounds. The mixed composition case induces a higher flux of neutrinos at
energies below 1013 eV due to the neutron decay component that extends down to
low energies. Detection of diffuse neutrino fluxes at ultra high energies can
strongly constrain the source distribution of UHECR whereas fluxes at lower
energies could be used to constrain confinement of VHE and UHE cosmic rays if
combined with composition analysis from cosmic ray experiments.
