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We re-examine the interesting possibility of utilizing the Glashow resonance(GR) channel nu_ebar + e^- to W^- to anything to discriminate between the UHEcosmic neutrinos originating from p-gamma and pp collisions in an opticallythin source of cosmic rays. We propose a general parametrization of the initialneutrino flavor composition by allowing the ratios Phi^{p gamma}_{pi^-}/Phi^{pgamma}_{pi^+} and Phi^{pp}_{pi^-}/Phi^{pp}_{pi^+} to slightly deviate fromtheir conventional values. A relationship between the typical source parameterkappa = (Phi^{p gamma}_{pi^+} + Phi^{p gamma}_{pi^-})/(Phi^{pp}_{pi^+} +Phi^{pp}_{pi^-} + Phi^{p gamma}_{pi^+} + Phi^{p gamma}_{pi^-}) and the workingobservable of the GR R_0 = Phi^T_{nu_ebar}/ (Phi^T_{nu_mu} + Phi^T_{nu_mu}) ata neutrino telescope is derived, and the numerical dependence of R_0 on kappais illustrated by taking account of the latest experimental data on threeneutrino mixing angles. It is shown that a measurement of R_0 is in principlepossible to identify the pure p-gamma interaction (kappa =1), the pure ppinteraction (kappa =0) or a mixture of both of them (0 < kappa < 1) at a givensource of UHE cosmic neutrinos. The event rate of the GR signal against thebackground is also estimated.

The Glashow resonance as a discriminator of UHE cosmic neutrinos originating from p-gamma and p-p collisions