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Effect of Reconnection Probability on Cosmic (Super)string Network Density
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abstract
We perform numerical simulations of cosmic string evolution with intercommuting probability $P$ in the range $5\times 10^{-3}\le P\le 1$, both in the matter and radiation eras, using a modified version of the Allen-Shellard code. We find that the dependence of the scaling density on $P$ is significantly different than the suggested $\rho\propto P^{-1}$ form. In particular, for probabilities greater than $P\simeq 0.1$, $\rho(1/P)$ is approximately flat, but for $P$ less than this value it is well-fitted by a power-law with exponent $0.6^{+0.15}_{-0.12}$. This shows that the enhancement of string densities due to a small intercommuting probability is much less prominent than initially anticipated. We interpret the flat part of $\rho(1/P)$ in terms of multiple opportunities for string reconnections during one crossing time, due to small-scale wiggles. We also propose a two-scale model incorporating the key physical mechanisms, which satisfactorily fits our results over the whole range of $P$ covered by the simulations.
Forward citations
Cited by 4 Pith papers
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Probing the gravitational wave background from cosmic strings with LISA
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Cosmic string gravitational wave backgrounds at LISA: I. Signal survey, template reconstruction, and model comparison
As provided, the manuscript body (random lasing) does not correspond to the abstract (cosmic string gravitational wave backgrounds at LISA), leaving the abstract's quantitative claims unsupported by any accessible text.
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Constraints on Cosmic Strings from the Curl-Mode CMB Lensing Power Spectrum measured by ACT DR6
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