Scaling properties of cosmological axion strings. (arXiv:1811.12678v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Martins_C/0/1/0/all/0/1">C. J. A. P. Martins</a>
There has been recent interest in the evolution and cosmological consequences
of global axionic string networks, and in particular in the issue of whether or
not these networks reach the scale-invariant scaling solution that is known to
exist for the simpler Goto-Nambu and Abelian-Higgs string networks. This is
relevant for determining the amount and spectrum of axions they produce. We use
the canonical velocity-dependent one-scale model for cosmic defect network
evolution to study the evolution of these global networks, confirming the
presence of deviations to scale-invariant evolution and in agreement with the
most recent numerical simulations. We also quantify the cosmological impact of
these corrections and discuss how the model can be used to extrapolate the
results of numerical simulations, which have a limited dynamic range, to the
full cosmological evolution of the networks, enabling robust predictions of
their consequences. Our analysis suggests that around the QCD scale, when the
global string network is expected to disappear and produce most of the axions,
the number of global strings per Hubble patch should be around $xisim4.2$,
but also highlights the need for additional high-resolution numerical
simulations.
There has been recent interest in the evolution and cosmological consequences
of global axionic string networks, and in particular in the issue of whether or
not these networks reach the scale-invariant scaling solution that is known to
exist for the simpler Goto-Nambu and Abelian-Higgs string networks. This is
relevant for determining the amount and spectrum of axions they produce. We use
the canonical velocity-dependent one-scale model for cosmic defect network
evolution to study the evolution of these global networks, confirming the
presence of deviations to scale-invariant evolution and in agreement with the
most recent numerical simulations. We also quantify the cosmological impact of
these corrections and discuss how the model can be used to extrapolate the
results of numerical simulations, which have a limited dynamic range, to the
full cosmological evolution of the networks, enabling robust predictions of
their consequences. Our analysis suggests that around the QCD scale, when the
global string network is expected to disappear and produce most of the axions,
the number of global strings per Hubble patch should be around $xisim4.2$,
but also highlights the need for additional high-resolution numerical
simulations.
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