Galactic Halos and rotating bosonic dark matter

TL;DR

This paper explores rotating bosonic dark matter halos as models for galactic dark matter, analyzing their properties and effects on galaxy rotation curves to explain observed orbital velocity flattening.

Contribution

It introduces rotating bosonic dark matter halos as extended analogs of bosonic stars and evaluates their potential to explain galactic rotation curves and dark matter distribution.

Findings

Rotating bosonic halos can produce flat galactic rotation curves.

Different bosonic star models contribute variably to galactic dynamics.

Proposed models may account for dark matter in dwarf and spiral galaxies.

Abstract

Rotating bosonic dark matter halos are considered as potential candidates for modeling dark matter in galactic halos. These bosonic dark matter halos can be viewed as a dilute and very extended version of bosonic stars, and the methods used for the calculation and analysis of the latter objects can be directly applied. Bosonic stars, a hypothetical type of astrophysical objects, are categorized into two primary families, based on the nature of the particles composing them: Einstein-Klein-Gordon stars and Proca stars. We examine various models from both families and the rotation curves which their contribution induces in different galaxies, to identify the most plausible candidates that explain the flattening of orbital velocities observed in galactic halos. By exploring different combinations of our dark matter models with observable galactic features, we propose an interesting source to compensate for the apparent lack of matter in dwarf and spiral galaxies, providing a possible explanation for this longstanding astronomical puzzle.