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Understanding the evolution and cosmological consequences of topologicaldefect networks requires a combination of analytic modeling and numericalsimulations. The canonical analytic model for defect network evolution is theVelocity-dependent One-Scale (VOS) model. For the case of cosmic strings, thishas so far been calibrated using small numbers of Goto-Nambu and field theorysimulations, in the radiation and matter eras, as well as in Minkowskispacetime. But the model is only as good as the available simulations, and itshould be extended as further simulations become available. In previous work wepresented a General Purpose Graphics Processing Unit implementation of theevolution of cosmological domain wall networks, and used it to obtain animproved VOS model for domain walls. Here we continue this effort, exploiting amore recent analogous code for local Abelian-Higgs string networks. Thesignificant gains in speed afforded by this code enabled us to carry out 1032field theory simulations of $512^3$ size, with 43 different expansion rates.This detailed exploration of the effects of the expansion rate on the networkproperties in turn enables a statistical separation of various dynamicalprocesses affecting the evolution of the network. We thus extend and accuratelycalibrate the VOS model for cosmic strings, including separate terms for energylosses due to loop production and scalar/gauge radiation. By comparing thisnewly calibrated VOS model with the analogous one for domain walls wequantitatively show that energy loss mechanisms are different for the two typesof defects.

Extending and Calibrating the Velocity dependent One-Scale model for Cosmic Strings with One Thousand Field Theory Simulations