Simulating Rotating Newtonian Universes
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arXiv
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| Main Authors: | , , , |
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| Format: | Preprint |
| Published: |
2024
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| _version_ | 1866909410525184000 |
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| author | Pál, Balázs Goh, Tze Rácz, Gábor Szapudi, István |
| author_facet | Pál, Balázs Goh, Tze Rácz, Gábor Szapudi, István |
| contents | We present the results of a novel type of numerical simulation that realizes a rotating Universe with a shear-free, rigid body rotation inspired by a Gödel-like metric. We run cosmological simulations of unperturbed glasses with various degrees of rotation in the Einstein-de Sitter and the $Λ$CDM cosmologies. To achieve this, we use the StePS N-body code capable of simulating the infinite Universe, overcoming the technical obstacles of classical toroidal (periodic) topologies that would otherwise prevent us from running such simulations. Results show a clear anisotropy between the polar and equatorial expansion rates with more than $1\%$ deviation from the isotropic case for maximal rotation without closed timeline curves within the horizon, $ω_{0} \approx 10^{-3}$ Gyr$^{-1}$; a considerable effect in the era of precision cosmology. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_00594 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Simulating Rotating Newtonian Universes Pál, Balázs Goh, Tze Rácz, Gábor Szapudi, István Cosmology and Nongalactic Astrophysics Computational Physics We present the results of a novel type of numerical simulation that realizes a rotating Universe with a shear-free, rigid body rotation inspired by a Gödel-like metric. We run cosmological simulations of unperturbed glasses with various degrees of rotation in the Einstein-de Sitter and the $Λ$CDM cosmologies. To achieve this, we use the StePS N-body code capable of simulating the infinite Universe, overcoming the technical obstacles of classical toroidal (periodic) topologies that would otherwise prevent us from running such simulations. Results show a clear anisotropy between the polar and equatorial expansion rates with more than $1\%$ deviation from the isotropic case for maximal rotation without closed timeline curves within the horizon, $ω_{0} \approx 10^{-3}$ Gyr$^{-1}$; a considerable effect in the era of precision cosmology. |
| title | Simulating Rotating Newtonian Universes |
| topic | Cosmology and Nongalactic Astrophysics Computational Physics |
| url | https://arxiv.org/abs/2412.00594 |