Type-I cosmic string network

TL;DR

This paper investigates the properties of Type-I cosmic string networks through numerical simulations, highlighting the influence of the gauge field and the parameter 2 on network density in an expanding universe.

Contribution

It provides a detailed analysis of how the gauge field and the parameter 2 affect the correlation length and density of Type-I cosmic string networks in the Abelian-Higgs model.

Findings

Correlation length depends strongly on 2.

Network density peaks at a specific 2 value for 2<1.

Expansion influences the densest configuration of the network.

Abstract

We study the network of Type-I cosmic strings using the field-theoretic numerical simulations in the Abelian-Higgs model. For Type-I strings, the gauge field plays an important role, and thus we find that the correlation length of the strings is strongly dependent upon the parameter \beta, the ratio between the self-coupling constant of the scalar field and the gauge coupling constant, namely, \beta=\lambda/2e^2. In particular, if we take the cosmic expansion into account, the network becomes densest in the comoving box for a specific value of \beta for \beta<1.