We elaborate further the µ-deformation-based approach to modeling dark matter, in addition to the earlier proposed use of µ-deformed thermodynamics. Herein, we construct µdeformed analogs of the Lane-Emden equation (for density profiles), and find their solutions. Using these, we plot the rotation curves for a number of galaxies. Different curves describing chosen galaxies are labeled by respective (differing) values of the deformation parameter µ. As result, the use of µ-deformation leads to improved agreement with observational data. For all the considered galaxies, the obtained rotation curves (labeled by µ) agree better with data, as compared to the well known Bose-Einstein condensate model results of T. Harko. Besides, for five of the eight cases of galaxies we find better picture for rotation curves than the corresponding Navarro-Frenk-White (NFW) curves. Possible physical meaning of the parameter µ, basic for this version of µ-deformation, is briefly discussed.
Though very popular, Bose-Einstein condensate models of dark matter have some difficulties. Here we propose the so-called µ-Bose gas model (µ-BGM) as a model of dark matter, able to treat weak points. Within µ-BGM, the µ-dependence of thermodynamics arises through the respective µ-calculus (it generalizes usual differential calculus) and enters the partition function, total number of particles, internal energy, etc. We study thermodynamic geometry of the µ-BGM and find singular behavior of (scalar) curvature, confirming Bose-like condensation. The critical temperature of condensation T (µ) c for µ = 0 is higher than the boson T c . We find other important virtues of µ-thermodynamics versus usual bosons and conclude: the condensate of µ-Bose gas can serve as (an effective) model of galactic-halos dark matter.
Stellar and gas kinematics of galaxies are a sensitive probe of the dark matter distribution in the halo. The popular fuzzy dark matter models predict the peculiar shape of density distribution in galaxies: specific dense core with sharp transition to the halo. Moreover, fuzzy dark matter predicts scaling relations between the dark matter particle mass and density parameters. In this work, we use a Bayesian framework and several dark matter halo models to analyse the stellar kinematics of galaxies using the Spitzer Photometry & Accurate Rotation Curves database. We then employ a Bayesian model comparison to select the best halo density model. We find that more than half of the galaxies prefer the fuzzy dark model against standard dark matter profiles (NFW, Burkert, and cored NFW). While this seems like a success for fuzzy dark matter, we also find that there is no single value for the particle mass that provides a good fit for all galaxies.
scite is a Brooklyn-based organization that helps researchers better discover and understand research articles through Smart Citations–citations that display the context of the citation and describe whether the article provides supporting or contrasting evidence. scite is used by students and researchers from around the world and is funded in part by the National Science Foundation and the National Institute on Drug Abuse of the National Institutes of Health.