Constraints on cosmic string tension imposed by the limit on the stochastic gravitational wave background from the European Pulsar Timing Array

Abstract

We investigate the constraints that can be placed on the cosmic string tension by using the current Pulsar Timing Array limits on the stochastic gravitational wave background (SGWB). We have developed a code to compute the spectrum of gravitational waves (GWs) based on the widely accepted one-scale model. In its simplest form the one-scale model allows one to vary: (i) the string tension, Gμ/c^2; (ii) the size of cosmic string loops relative to the horizon at birth, α; (iii) the spectral index of the emission spectrum, q; (iv) the cut-off in the emission spectrum, n_*; and (v) the intercommutation probability, p. The amplitude and slope of the spectrum in the nHz frequency range is very sensitive to these unknown parameters. We have also investigated the impact of more complicated scenarios with multiple initial loop sizes, in particular the 2-αmodels proposed in the literature and a log-normal distribution for α. We have computed the constraint on Gμ/c^2 due to the limit on a SGWB imposed by data from the European Pulsar Timing Array. Taking into account all the possible uncertainties in the parameters we find a conservative upper limit of Gμ/c^2<5.3x 10^{-7} which typically occurs when the loop production scale is close to the gravitational backreaction scale, α\approxΓGμ/c^2. Stronger limits are possible for specific values of the parameters which typically correspond to the extremal cases α\ll ΓGμ/c^2 and α\gg ΓGμ/c^2. This limit is less stringent than the previously published limits which are based on cusp emission, an approach which does not necessarily model all the possible uncertainties. We discuss the prospects for lowering this limit by two orders of magnitude, or even a detection of the SGWB, in the very near future in the context of the Large European Array for Pulsars and the Square Kilometre Array.

24 pages, 14 figures, accepted for publication in Physical Review D. Minor corrections and additional comments - updated to match the published version

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