Detection of Low Tension Cosmic Superstrings
  Cosmic superstrings of string theory differ from conventional cosmic strings
of field theory. We review how the physical and cosmological properties of the
macroscopic string loops influence experimental searches for these relics from
the epoch of inflation. The universe's average density of cosmic superstrings
can easily exceed that of conventional cosmic strings having the same tension
by two or more orders of magnitude. The cosmological behavior of the remnant
superstring loops is qualitatively distinct because the string tension is
exponentially smaller than the string scale in flux compactifications in string
theory. Low tension superstring loops live longer, experience less recoil
(rocket effect from the emission of gravitational radiation) and tend to
cluster like dark matter in galaxies. Clustering enhances the string loop
density with respect to the cosmological average in collapsed structures in the
universe. The enhancement at the Sun's position is $\sim 10^5$. We develop a
model encapsulating the leading order string theory effects, the current
understanding of the string network loop production and the influence of
cosmological structure formation suitable for forecasting the detection of
superstring loops via optical microlensing, gravitational wave bursts and fast
radio bursts. We evaluate the detection rate of bursts from cusps and kinks by
LIGO- and LISA-like experiments. Clustering dominates rates for $G \mu <
10^{-11.9}$ (LIGO cusp), $G \mu<10^{-11.2}$ (LISA cusp), $G \mu < 10^{-10.6}$
(LISA kink); we forecast experimentally accessible gravitational wave bursts
for $G \mu>10^{-14.2}$ (LIGO cusp), $G \mu>10^{-15}$ (LISA cusp) and $G
\mu>10^{- 14.1}$ (LISA kink).
