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      Non-Linear Axion Dynamics and Formation of Cosmological Pseudo-Solitons

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          Abstract

          The \((3+1)\)-dimensional evolution of an inhomogeneous axion field configuration around the QCD epoch is studied numerically, including important non-linear effects due to the attractive self-interaction. It is found that axion perturbations on scales corresponding to causally disconnected regions at \(T \sim 1 \, {\rm GeV}\) can lead to very dense pseudo-soliton configurations we call axitons. These configurations evolve to axion miniclusters with present density \(\rho_a \ga 10^{-8}\,{\rm g \, cm^{-3}}\). This is high enough for the collisional \(2a \rightarrow 2a\) process to lead to Bose--Einstein relaxation in the gravitationally bound clumps of axions, forming Bose stars.

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          QCD and instantons at finite temperature

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            Astrophysical methods to constrain axions and other novel particle phenomena

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              Cosmic and local mass density of ‘‘invisible’’ axions

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                Author and article information

                Journal
                15 November 1993
                Article
                10.1103/PhysRevD.49.5040
                astro-ph/9311037
                f00de619-a2d9-4548-8d34-2371c43162c2
                History
                Custom metadata
                Phys.Rev.D49:5040-5051,1994
                27 pages plus 13 figures (upon request: rocky@fnas01.fnal.gov), LaTeX, FNAL--PUB--93/335--A
                astro-ph gr-qc hep-ph

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