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- W2108182512 abstract "The equation which governs the temporal evolution of a gravitational wave (GW) in curved space-time can be treated as the Schrodinger equation for a particle moving in the presence of an effective potential. When GWs propagate in an expanding universe with constant effective potential, there is a critical value $({k}_{c})$ of the comoving wave number which discriminates the metric perturbations into oscillating $(k>{k}_{c})$ and nonoscillating $(k<{k}_{c})$ modes. As a consequence, if the nonoscillatory modes are outside the horizon they do not freeze out. The effective potential is reduced to a nonvanishing constant in a cosmological model which is driven by a two-component fluid, consisting of radiation (dominant) and cosmic strings (subdominant). It is known that the cosmological evolution gradually results in the scaling of a cosmic-string network and, therefore, after some time $(ensuremath{Delta}ensuremath{tau})$ the Universe becomes radiation dominated. The evolution of the nonoscillatory GW modes during $ensuremath{Delta}ensuremath{tau}$ (while they were outside the horizon), results in the distortion of the GW power spectrum from what it is anticipated in a pure radiation model, at present-time frequencies in the range ${10}^{ensuremath{-}16}text{ }text{ }mathrm{Hz}<fensuremath{lesssim}{10}^{5}text{ }text{ }mathrm{Hz}$." @default.
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- W2108182512 date "2008-07-16" @default.
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- W2108182512 title "Imprints of cosmic strings on the cosmological gravitational wave background" @default.
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- W2108182512 doi "https://doi.org/10.1103/physrevd.78.024027" @default.
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