Imprints of cosmic strings on the cosmological gravitational wave background

Details Imprints of cosmic strings on the cosmological gravitational wave background Imprints of cosmic strings on the cosmological gravitational wave background

2008-06-18

arxiv.org/abs/0806.2999v1

Phys.Rev.D78:024027,2008

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

8 pages, 1 figure, accepted for publication to Physical Review D

Scientific paper

10.1103/PhysRevD.78.024027

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 non-oscillating (k < k_c) modes. As a consequence, if the non-oscillatory modes are outside the horizon they do not freeze out. The effective potential is reduced to a non-vanishing constant in a cosmological model which is driven by a two-component fluid, consisting of radiation (dominant) and cosmic strings (sub-dominant). It is known that the cosmological evolution gradually results in the scaling of a cosmic-string network and, therefore, after some time (\Dl \ta) the Universe becomes radiation-dominated. The evolution of the non-oscillatory GW modes during \Dl \ta (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^{-16} Hz < f < 10^5 Hz.

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