1994/03/02 by Julian Borrill, Edmund J Copeland, Edmund J. Copeland +5
Mathematics · Physics and Astronomy · #Anisotropy #Computational physics #Core (optical fiber) #Cosmic microwave background #Cosmology and Gravitation Theories #Event (particle physics) #Field (mathematics) #Galaxies: Formation, Evolution, Phenomena #Image (mathematics) #Mathematics #Nonlinear system #Optics #Physics #Pure mathematics #Quantum mechanics #Radio Astronomy Observations and Technology #Sigma #Sigma model #Statistical physics #Texture (cosmology) #Work (physics) #astro-ph
paper · pdf · doi:10.1103/physrevd.50.2469
published as Phys.Rev. D50 (1994) 2469-2478 · 15 pages, standard LaTeX with 5 postscript figures available on request, SUSSEX-AST 94/3-1
arxiv created 1994/03/02 · openalex publication_date 1994/08/15 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We use numerical simulations to calculate the cosmic microwave background anisotropy induced by the evolution of a global texture field, with special emphasis on individual textures. Both spherically symmetric and general configurations are analyzed, and in the latter case we consider field configurations which exhibit unwinding events and also ones which do not. We compare the results given by evolving the field numerically under both the expanded core (XCORE) and nonlinear \ensuremathσ model (NLSM) approximations with the analytic predictions of the NLSM exact solution for a spherically symmetric self-similar (SSSS) unwinding. We find that the random unwinding configuration spots' typical peak height is 60--75 % and angular size typically only 10% of those of the SSSS unwinding, and that random configurations without an unwinding event nonetheless may generate indistinguishable hot and cold spots. A brief comparison is made with other work.