2021/07/31 by Iskander G. Abdullin, Vladimir A. Popov, V. А. Popov
Chemistry · Physics and Astronomy · #Astrophysics #Boson #Cold Atom Physics and Bose-Einstein Condensates #Dark matter #Dark matter halo #Galactic halo #Galaxy #Galaxy rotation curve #Halo #Particle physics #Physics #Quantum, superfluid, helium dynamics #Spectroscopy and Laser Applications #astro-ph.GA #gr-qc #hep-ph
paper · pdf · doi:10.1088/1475-7516/2021/11/055
31 pages, 5 figures, 2 tables
openalex publication_date 2021/11/01 · arxiv created 2021/11/07 · arxiv updated 2021/12/08 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We consider galaxy halos formed by dark matter bosons with mass in the range of about a few tens or hundreds eV. A major part of the particles is in a noncondensed state and described under the Thomas-Fermi approach. Derived equations are solved numerically to find the halo density profile. The noncondensed state is supported in the entire halo except compact gravitationally bounded Bose-Einstein condensates. Although the size of these compact objects, also known as Bose stars, depends on interactions between the particles, its upper limit is only about 100 astronomical units. The Bose stars collect the condensed bosons providing a density cusp avoidance in the halo as well as a natural mechanism to prevent overproduction of small halos. Clusters of the Bose stars can also contribute to the halo density profile. The model is analyzed by confronting its predictions with observations of galaxy rotation curves. We employ 22 low surface brightness galaxies and obtain that the model is consistent with the observational data when the particle mass is in the range above about 50 eV and the best fit corresponds to the mass m = 86 eV. This mass is appropriate for relic dark matter bosons, which decouple just after QCD phase transition.