Gravitational radiation from cosmic (super)strings: bursts, stochastic background, and observational windows

TL;DR

This paper reexamines gravitational wave signals from cosmic (super)strings, analyzing how parameters like reconnection probability and loop size affect observable signatures, and finds that previous results are generally robust.

Contribution

It investigates the impact of reconnection probability and loop size on gravitational wave signals from cosmic strings, extending previous models to superstring scenarios.

Findings

GW burst signals are robust against parameter variations.

Stochastic GW background remains detectable under certain conditions.

Pulsar timing data may contain signatures of transient GW bursts.

Abstract

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.