File:Clusters.png
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Summary
Evolution of a density contrast of an overdense cosmic region. Comparison between the linear approximation (LA) and the Szekeres solution (SZ) reveals how quickly the evolution of cosmic structures becomes non-linear and needs to be traced using the exact methods. 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].
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| Date/Time | Thumbnail | Dimensions | User | Comment | |
|---|---|---|---|---|---|
| current | 09:38, 24 February 2015 | | 1,000 × 700 (70 KB) | Krzysztof Bolejko (Talk | contribs) | Reverted to version as of 09:31, 24 February 2015 |
| 09:37, 24 February 2015 |  | 1,000 × 700 (70 KB) | Krzysztof Bolejko (Talk | contribs) | Evolution of a density contrast of an overdense cosmic region. Comparison between the linear approximation (LA) and the Szekeres solution (SZ) reveals how quickly the evolution of cosmic structures becomes non-linear and needs to be traced using the ex... | |
| 09:31, 24 February 2015 |  | 1,000 × 700 (70 KB) | Krzysztof Bolejko (Talk | contribs) | Evolution of a density contrast of an overdense cosmic region. Comparison between the linear approximation (LA) and the Szekeres solution (SZ) reveals how quickly the evolution of cosmic structures becomes non-linear and needs to be traced using the ex... |
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