Evolution of a density contrast of a cosmic void using the linear approximation (LA) and the Szekeres model (SZ). In both cases the initial conditions are the same. As seen the evolution of cosmic voids quickly enters the non-linear regime. This happens quite early in the Universe evolution, less than 500 My after the Big Bang. After 2,000 My the linear approximation completely breaks down predicting unphysical values of the density contrast (the density contrast cannot have values that are less than -1). When referring to this figure, please also cite [Bolejko,Phys.Rev.D73:123508,2006, http://arxiv.org/abs/astro-ph/0604490v2] and [Bolejko,Phys.Rev.D75:043508,2007, http://arxiv.org/abs/astro-ph/0610292].
This work is licensed under the Creative Commons Attribution 3.0 License.
Click on a date/time to view the file as it appeared at that time.
|current||07:41, 24 February 2015||1,000 × 700 (62 KB)||Krzysztof Bolejko||Evolution of a density contrast of a cosmic void using the linear approximation (LA) and the Szekeres solution (SZ).|