Scaling of cosmic string loops

Vanchurin, Vitaly; Olum, Ken D.; Vilenkin, Alexander

doi:10.1103/physrevd.74.063527

Cited by 198 publications

(280 citation statements)

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“…The scaling regime of string loops appears after a transient relaxation era, driven by a transient overproduction of string loops with length close to the initial correlation length of the string network. Subsequently, numerical [18] and analytical [19] studies supported the results of Ref. [17].…”

Section: Cosmic String Dynamicssupporting

confidence: 65%

Cosmic Strings and Cosmic Superstrings

Sakellariadou

2009

Nuclear Physics B - Proceedings Supplements

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In these lectures, I review the current status of cosmic strings and cosmic superstrings. I first discuss topological defects in the context of Grand Unified Theories, focusing in particular in cosmic strings arising as gauge theory solitons. I discuss the reconciliation between cosmic strings and cosmological inflation, I review cosmic string dynamics, cosmic string thermodynamics and cosmic string gravity, which leads to a number of interesting observational signatures. I then proceed with the notion of cosmic superstrings arising at the end of brane inflation, within the context of brane-world cosmological models inspired from string theory. I discuss the differences between cosmic superstrings and their solitonic analogues, I review our current understanding about the evolution of cosmic superstring networks, and I then briefly describe the variety of observational consequences, which may help us to get an insight into the stringy description of our Universe.

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Section: Cosmic String Dynamicssupporting

confidence: 65%

Cosmic Strings and Cosmic Superstrings

Sakellariadou

2009

Nuclear Physics B - Proceedings Supplements

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“…(2.11) was indeed originally obtained in such simulations [37], but we are not aware of any results indicating that ξ(t) ∼ L(t) in this regime. On the contrary, preliminary results of a new, high-resolution flat-space simulation indicate that ξ(t) is substantially larger than L(t) [38].…”

Section: A Standard Scenariomentioning

confidence: 90%

Gravitational radiation from cosmic (super)strings: Bursts, stochastic background, and observational windows

2005

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The gravitational wave (GW) signals emitted by a network of cosmic strings are reexamined in view of the possible formation of a network of cosmic superstrings at the end of brane inflation. The reconnection probability p of intersecting fundamental or Dirichlet strings might be much smaller than 1, and the properties of the resulting string network may differ significantly from those of ordinary strings (which have p = 1). In addition, it has been recently suggested that the typical length of newly formed loops may differ by a factor ǫ ≪ 1 from its standard estimate. Here, we analyze the effects of the two parameters p and ǫ on the GW signatures of strings. We consider both the GW bursts emitted from cusps of oscillating string loops, which have been suggested as candidate sources for the LIGO/VIRGO and LISA interferometers, and the stochastic GW background, which may be detectable by pulsar timing observations. In both cases we find that previously obtained results are quite robust, at least when the loop sizes are not suppressed by many orders of magnitude relative to the standard scenario. We urge pulsar observers to reanalyze a recently obtained 17-year combined data set to see whether the large scatter exhibited by a fraction of the data might be due to a transient GW burst activity of some sort, e.g. to a near cusp event.

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“…This is the maximum size of the loops. According to the recent computer simulations of string networks [54][55][56], the typical initial size of the loops is governed by the cosmic time t when they are produced, L max αt with α ∼ 0.1. The parameter ξ is also determined by dynamics of cosmic string network.…”

Section: Jhep01(2014)049mentioning

confidence: 99%