  The gravitational wave (GW) signals emitted by a network of cosmic strings
are reexamined in view of the possible formation of a network of cosmic
superstrings at the end of brane inflation. The reconnection probability $p$ of
intersecting fundamental or Dirichlet strings might be much smaller than 1, and
the properties of the resulting string network may differ significantly from
those of ordinary strings (which have $p=1$). In addition, it has been recently
suggested that the typical length of newly formed loops may differ by a factor
$\epsilon \ll 1$ from its standard estimate. Here, we analyze the effects of
the two parameters $p$ and $\epsilon$ on the GW signatures of strings. We
consider both the GW bursts emitted from cusps of oscillating string loops,
which have been suggested as candidate sources for the LIGO/VIRGO and LISA
interferometers, and the stochastic GW background, which may be detectable by
pulsar timing observations. In both cases we find that previously obtained
results are \textit{quite robust}, at least when the loop sizes are not
suppressed by many orders of magnitude relative to the standard scenario. We
urge pulsar observers to reanalyze a recently obtained 17-year combined data
set to see whether the large scatter exhibited by a fraction of the data might
be due to a transient GW burst activity of some sort, e.g. to a near cusp
event.
