Constraining Bose-Einstein condensate dark matter models with the galaxy rotation curves of the SPARC sample

Abstract

If dark matter did exist in the form of a self-interacting boson gas, when its temperature became lower than the critical, density dependent temperature, a phase transition to a Bose-Einstein Condensate did occur in the early Universe. The presence of the condensate dark matter leads to specific signatures in the galaxy rotation, and in the dark matter density distribution. In particular Bose-Einstein Condensate (BEC) dark matter models predict a finite and well defined radius of the dark matter halo, whose numerical value depends on the mass of the dark matter particle, and of the scattering length.

We compare the theoretical predictions of the functional form of the rotation curves in the slowly rotating BEC models with the SPARC sample of measured rotation curves, by using genetic algorithms, to fit the observational data, and to obtain estimates of the relevant physical parameters of the BEC dark matter halos (central density, angular velocity and static radius).

The density profiles of the dark matter distribution are also considered, and it follows that the presence of the condensate dark matter could also provide an alternative solution for the core/cusp problem.

Authors

M. Crăciun
(Tiberiu Popoviciu Institute of Numerical Analysis)

T. Harko
(Department of Physics, Babes-Bolyai University, Cluj-Napoca, Romania and
School of Physics, Sun Yat-Sen University Guangzhou, People’s Republic of China)

Keywords

Cosmology; galactic astronomy; dark matter; Bose-Einstein condensation

References

See the expanding block below.

Paper coordinates

M. Crăciun, T. Harko, Constraining Bose-Einstein condensate dark matter models with the galaxy rotation curves of the SPARC sample, Romanian Astronomical Journal, 29 (2019) no.2, 101-118.

PDF

http://www.astro.ro/~roaj/29_2/11-craciun.pdf

About this paper

Journal

Romanian Astronomical Journal

Publisher Name

Romanian Academy Publishing House (Editura Academiei Romane)

DOI

not available yet.

Print ISSN

1220-5168  

Online ISSN

2285-3758

Google Scholar Profile

not available yet

References

References

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