Evolution and dynamical properties of Bose-Einstein condensate dark matter stars

Abstract

Using recently developed nonrelativistic numerical simulation code, we investigate the stability properties of compact astrophysical objects that may be formed due to the Bose-Einstein condensation of dark matter. Once the temperature of a boson gas is less than the critical temperature, a Bose-Einstein condensation process can always take place during the cosmic history of the universe. Due to dark matter accretion, a Bose-Einstein condensed core can also be formed inside massive astrophysical objects such as neutron stars or white dwarfs, for example. Numerically solving the Gross-Pitaevskii-Poisson system of coupled differential equations, we demonstrate, with longer simulation runs, that within the computational limits of the simulation the objects we investigate are stable. Physical properties of a self-gravitating Bose-Einstein condensate are examined both in non-rotating and rotating cases.

9 pages, 3 figures

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• Condensate dark matter stars
• Numerical simulation code for self-gravitating Bose-Einstein condensates
• Boson star at finite temperature
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• DMAW 2010 LEGACY the Presentation Review: Dark Matter in Galaxies with its Explanatory Notes
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• A review on radiation of oscillons and oscillatons
• Compact stars admitting Finch-Skea symmetry in the presence of various matter fields
• Bose-Einstein Condensate dark matter models in the presence of baryonic matter and random confining potentials
• Dynamical galactic effects induced by stable vortex structure in bosonic dark matter
• Pale Glares of Dark Matter in Quantum Spacetime
• Fundamental fields around compact objects: Massive spin-2 fields, Superradiant instabilities and Stars with dark matter cores
• The Gross-Pitaevskii-Poisson model for an ultracold plasma: density waves and solitons