Erratum: Scaling of multitension cosmic superstring networks [Phys. Rev. DPRVDAQ0556-282171, 103508 (2005)]

Abstract

Brane inflation in superstring theory ends when branes collide, initiating the hot big bang.Cosmic superstrings are produced during the brane collision. The cosmic superstrings produced in a D3-brane-antibrane inflationary scenario have a spectrum: (p, q) bound states of p fundamental (F) strings and q D-strings, where p and q are coprime. By extending the velocity-dependent onescale network evolution equations for abelian Higgs cosmic strings to allow a spectrum of string tensions, we construct a coupled (infinite) set of equations for strings that interact through binding and self-interactions. We apply this model to a network of (p, q) superstrings. Our numerical solutions show that (p, q) networks rapidly approach a stable scaling solution. We also extract the relative densities of each string type from our solutions. Typically, only a small number of the lowest tension states are populated substantially once scaling is reached. The model we study also has an interesting new feature: the energy released in (p, q) string binding is by itself adequate to allow the network to reach scaling. This result suggests that the scaling solution is robust.To demonstrate that this result is not trivial, we show that choosing a different form for string interactions can lead to network frustration.

Scaling properties of multitension domain wall networks

“…By studying the asymptotic scaling properties of these networks in generic expanding universes we have confirmed two classes of solutions: one corresponds to the well-known linear scaling solution, while the other corresponds to the case where the curvature is concentrated in the wall junctions. Our results complement those for cosmic strings [18,19], though we emphasize that the way we model the network is slightly different and aims to model the properties that are more easily measurable in field theory numerical simulations.…”

“…The purpose of this model is to describe the interaction between the different types of defects, in order to determine if this kind of networks can reach a scaling regime, as suggested in [18,19]. Additional motivation for working with three types of walls is also provided by [19], who find that in the case of cosmic strings the three lightest components dominate the dynamics, with the heavier ones being suppressed.…”

“…This assumption (not explicitly enforced by [18]) is a conservative approach when it comes to scaling. For simplicity we only consider energy transfers from two types of walls to the third one, but we have checked that our general results would still hold if all possible energy transfers were allowed.…”

“…Our main interest is on the conditions under which a scale-invariant evolution of the network (whose presence for the simplest walls is well established, both on analytic and numerical grounds) still applies, but we will also consider a physically interesting low-curvature limit. The goal is to use this information to shed light on the analogous case for cosmic strings, in which case the issue of the generality of the scale-invariant asymptotic evolution is still not fully clear, although several analytic [13,18,19] and numerical efforts [12,[20][21][22] suggest that it applies in a wide range of circumstances.…”

Brane world cosmic string interaction

“…Firstly, it has been shown that it is possible for non-intercommuting strings to reach a scaling solution [7]. Furthermore, a careful study of Type I strings reveals that in fact they do intercommute, except when the angle between the colliding strings is small [3,8].…”