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UHE neutrinos with $E>10^{17}$ eV can be produced by ultra-high energy cosmicrays (UHECR) interacting with CMB photons (cosmogenic neutrinos) and bytop-down sources, such as topological defects (TD), superheavy dark matter(SHDM) and mirror matter. Cosmogenic neutrinos are reliably predicted and theirfluxes can be numerically evaluated using the observed flux of UHECR. The lowerlimit for the flux is obtained for the case of pure proton composition of theobserved UHECR. The rigorous upper limit for cosmogenic neutrino flux alsoexists. The maximum neutrino energy is determined by maximum energy ofacceleration, which at least for the shock acceleration is expected not toexceed $10^{21} - 10^{22}$ eV. The top-down sources provide neutrino energies afew orders of magnitude higher, and this can be considered as a signature ofthese models. Oscillations play important role in UHE neutrino astronomy. Atproduction of cosmogenic neutrinos $\tau$-neutrinos are absent and$\bar{\nu}_e$ neutrinos are suppressed. These species, important for detection,appear in the observed fluxes due to oscillation. Mirror neutrinos cannot beobserved directly, but due to oscillations to ordinary neutrinos they canprovide the largest neutrino flux at the highest energies.

UHE neutrino astronomy and neutrino oscillations