2011/04/26 by Yosuke Misonoh, Kei-ichi Maeda, Kei Maeda +1
Physics and Astronomy · #Astrophysics #Big Bang (financial markets) #Big Crunch #Big Rip #Black Holes and Theoretical Physics #Context (archaeology) #Cosmological constant #Cosmology #Cosmology and Gravitation Theories #Dark energy #De Sitter universe #Flatness problem #Galaxies: Formation, Evolution, Phenomena #Mathematical physics #Metric expansion of space #Particle horizon #Physical cosmology #Physics #Steady State theory #Theoretical physics #Ultimate fate of the universe #Universe #astro-ph.CO #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.84.064030
published as Phys.Rev.D84:064030,2011 · 18 pages, 21 figures, 5 tables
arxiv created 2011/04/26 · openalex publication_date 2011/09/20 · arxiv updated 2015/03/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study a vacuum Bianchi IX universe in the context of Ho\ifmmode \checkr\else \vr\fiava-Lifshitz gravity. In particular, we focus on the classical dynamics of the universe and analyze how anisotropy changes the history of the universe. For small anisotropy, we find an oscillating universe as well as a bounce universe just as the case of the Friedmann-Lemaitre-Robertson-Walker spacetime. However, if the initial anisotropy is large, we find the universe which ends up with a big crunch after oscillations if a cosmological constant \ensuremathΛ is zero or negative. For \ensuremathΛ>0, we find a variety of histories of the universe, that is a de Sitter expanding universe after oscillations in addition to the oscillating solution and the previous big crunch solution. This fate of the universe shows sensitive dependence of initial conditions, which is one of the typical properties of a chaotic system. If the initial anisotropy is near the upper bound, we find the universe starting from a big bang and ending up with a big crunch for \ensuremathΛ\ensuremath≤0, and a de Sitter expanding universe starting from a big bang for \ensuremathΛ>0.