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Defect Evolution in Cosmology and Condensed Matter: by C.J.A.P. Martins

By C.J.A.P. Martins

This booklet sheds new mild on topological defects in broadly differing structures, utilizing the Velocity-Dependent One-Scale version to higher comprehend their evolution. Topological defects – cosmic strings, monopoles, area partitions or others - inevitably shape at cosmological (and condensed subject) section transitions. in the event that they are strong and long-lived they are going to be fossil relics of higher-energy physics. figuring out their behaviour and effects is a key a part of any severe try to comprehend the universe, and this calls for modelling their evolution. The velocity-dependent one-scale version is the single absolutely quantitative version of illness community evolution, and the canonical version within the box. This publication presents a evaluate of the version, explaining its actual content material and describing its huge diversity of applicability.

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Additional resources for Defect Evolution in Cosmology and Condensed Matter: Quantitative Analysis with the Velocity-Dependent One-Scale Model (SpringerBriefs in Physics)

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There are two values of εr 2 for which σd = 2σe : εr 2 = 0 and εr 2 = −1. Thus for εr 2 > 0 and εr 2 < −1 Y-type junctions are favored while for −1 < εr 2 < 0 X-type junctions are preferred. In passing, we note that the parameter ε determines not only the ratio of the energies in the two sectors, but also influences, among other things, how fast the unstable junctions will decay into the stable ones. These expectations have been confirmed numerically. Note that the particular cases εr 2 = 0 and εr 2 = −1 do not represent marginal cases between the formation of the junctions of the type Y and X.

74) dt dt leading to d(γ v) kγ γv = − dt R d (4 − n) dLph Lph 1 = (4 − n)HLph + kv + γ 4−n cv. 77) dt Lph d (4 − n) dLph 1 = (4 − n)HLph + v(k + c)γ 4−n . 78) Note that the damping length scale does not appear in the evolution equation for the physical length scale, but only in the one for the invariant length scale (as well as in the one for the velocity). 79) which is trivially correct and consistent given the various definitions above. We can also confirm how the model parameters c and k behave as one switches between the physical and invariant approaches.

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