Abstract

Cosmic superstrings are line-like objects of cosmic size which are predicted to form at the end of brane inflation in a number of string motivated models. As opposed to their field theory counterparts (“standard” cosmic strings), cosmic superstrings are thought to exist in different varieties, with a spectrum of tensions; the different strings types can meet at Y-junctions; and strings interact with each-other and themselves in new ways. These different tensions and interactions depend on the parameters of the underling superstring theory, namely $\mu_F$ and $g_s$, the fundamental string tension and coupling. Observational signatures of cosmic superstrings will therefore depend on $(\mu_F, g_s)$, with different signatures being sensitive to different combinations of these parameters. Therefore the hope is that via (at least two) observations, the parameters $\mu_F$ and $g_s$ could be pinned down. In this talk, after a brief discussion of the evolution of cosmic superstring networks with junctions, I will focus on their GW and CMB signatures (particularly discussing how these differ from those of “standard” cosmic strings). I will show how these signatures depend on the underlying parameters.