  We present projected constraints on the cosmic string tension, $G\mu/c^2$,
that could be achieved by future gravitational wave detection experiments and
express our results as semi-analytic relations of the form $G\mu(\Omega_{\rm
gw}h^2)/c^2$, to allow for direct computation of the tension constraints for
future experiments. These results can be applied to new constraints on $\ogwh$
as they are imposed. Experiments operating in different frequency bands probe
different parts of the gravitational wave spectrum of a cosmic string network
and are sensitive to different uncertainties in the underlying cosmic string
model parameters. We compute the gravitational wave spectra of cosmic string
networks based on the one-scale model, covering all the parameter space
accessed by each experiment which is strongly dependent on the birth scale of
loops relative to the horizon, $\alpha$. The upper limits on the string tension
avoid any assumptions on the model parameters. We perform this investigation
for Pulsar Timing Array experiments of different durations as well as
ground-based and space-borne interferometric detectors.
