Relic gravitational waves from cosmic strings: Updated constraints and opportunities for detection.

We examine the spectrum of gravitational radiation emitted by a network of cosmic strings, with emphasis on the observational constraints and the opportunities for detection. The analysis improves over past work, as we use a phenomenological model for the radiation spectrum emitted by a cosmic string loop. This model attempts to include the effect of the gravitational back reaction on the radiation emission by an individual loop with a high frequency cutoff in the spectrum. Comparison of the total spectrum due to a network of strings with the recently improved bound on the amplitude of a stochastic gravitational wave background, due to measurements of noise in pulsar signal arrival times, allows us to exclude a range of values of $\ensuremath{\mu}$, the cosmic string linear mass density, for certain values of cosmic string and cosmological parameters. We find the conservative bound $\frac{G\ensuremath{\mu}}{{c}^{2}}l5.4(\ifmmode\pm\else\textpm\fi{}1.1)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}6}$ which is consistent with all other limits. We consider variations of the standard cosmological scenario, finding that an underdense, ${\ensuremath{\Omega}}_{0}l1$ universe has little effect on the spectrum, whereas the portion of the spectrum probed by gravitational wave detectors is strongly sensitive to the thermal history of the cosmological fluid. We discuss the opportunity for the observation of this stochastic background by resonant mass and laser interferometer gravitational wave detectors.