Evolution of cosmological perturbations in Bose–Einstein condensate dark matter
By Tiberiu Harko. 2011
157 citations recorded by the source corpus.
We consider the global cosmological evolution and the evolution of the density contrast in the Bose-Einstein condensate dark matter model, in the framework of a PostNewtonian cosmological approach. In the Bose-Einstein model, dark matter can be described as a non-relativistic, Newtonian gravitational condensate, whose density and pressure are related by a barotropic equation of state. For a condensate with quartic non-linearity, the equation of state is polytropic with index n = 1.The basic equation describing the evolution of the perturbations of the Bose-Einstein condensate is obtained, and its solution is studied by using both analytical and numerical methods. The global cosmological evolution as well as the evolution of the perturbations of the condensate dark matter shows significant differences with respect to the pressureless dark matter model, considered in the framework of standard cosmology. Therefore the presence of condensate dark matter could have modified drastically the cosmological evolution of the early universe, as well as the large scale structure formation process.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics
View Paper: https://www.semanticscholar.org/paper/77fbb39c56536fdc4e6130904aab10cb7980be27
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Citations in the corpus
- Angular Momentum and Vortex Formation in Bose-Einstein-Condensed Cold Dark Matter Haloes (2011, result): “Some recent results on structure formation studies involving BEC-CDM can be found in the works of Ureña-López & Guzmán (2003); Fukuyama, Morikawa & Tatekawa (2008); Woo & Chiueh (2009); Marsh & Ferreira (2010); Harko (2011) and Chavanis (2012)3.”
- Growth of perturbations in an expanding universe with Bose-Einstein condensate dark matter (2011, methodology): “When k > 0, which is the case previously considered by Harko (2011), the density exists only for a > a∗ = (kA) 1/3.”