Cosmic Strings and Their Induced Non-Gaussianities in the Cosmic Microwave Background

Figure 10

Loop energy density distribution with respect of the conformal time for the smallest loops. By the end of the numerical simulation, these loops have not yet reached their scaling behaviour (a). (b) is the corresponding loop number density distribution at the end of the simulation (). Compared to the asymptotic scaling power law (red dashed), the loops in the relaxation regime are preferentially produced at fixed physical lengths given by the initial correlations present in the VV network.

(a)

(b)