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

TL;DR

This paper uses numerical simulations to study the stability and physical properties of Bose-Einstein condensate dark matter stars, including their formation, rotation, and potential presence inside other astrophysical objects.

Contribution

It provides the first detailed numerical analysis of the stability and properties of Bose-Einstein condensate dark matter stars using the Gross-Pitaevskii-Poisson system.

Findings

Objects studied are stable within simulation limits.

Physical properties examined in rotating and non-rotating cases.

Condensed cores can form inside neutron stars or white dwarfs.

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.