Evolution of cosmic strings

Details Evolution of cosmic strings Evolution of cosmic strings

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985phrvl..54.1868a&link_type=abstract

Physical Review Letters (ISSN 0031-9007), vol. 54, April 22, 1985, p. 1868-1871. Research supported by the Robert A. Welsh Found

Statistics

Computation

242

Cosmology, String Theory, Unified Field Theory, Brownian Movements, Computational Astrophysics, Density Wave Model, Energy Distribution

Scientific paper

Preliminary results from numerical simulations of the time evolution of cosmic strings formed as defect lines in the orientation of the Higgs field mediating the phase transition in the very early universe are reported. The equations of motion for infinitely thin directional relativistic strings in a spatially flat radiation-dominated universe are modeled for the cases p = 1 and p = 0, where p is the probability that two strings intercommute when they cross and 1-p is the probability that they pass through each other, and for initial coherence lengths approximately equal to the horizon scale. The results are presented graphically, and it is found that for p = 1 the string energy density scales as radiation and does not become dominant.

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