Hydrodynamics of galactic dark matter

Details Hydrodynamics of galactic dark matter Hydrodynamics of galactic dark matter

2001-12-19

arxiv.org/abs/gr-qc/0112044v2

Class.Quant.Grav. 19 (2002) 3603-3616

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

LaTeX article style, 16 pages including three figures. Final version to appear in Classical and Quantum Gravity

Scientific paper

10.1088/0264-9381/19/14/303

We consider simple hydrodynamical models of galactic dark matter in which the galactic halo is a self-gravitating and self-interacting gas that dominates the dynamics of the galaxy. Modeling this halo as a sphericaly symmetric and static perfect fluid satisfying the field equations of General Relativity, visible barionic matter can be treated as ``test particles'' in the geometry of this field. We show that the assumption of an empirical ``universal rotation curve'' that fits a wide variety of galaxies is compatible, under suitable approximations, with state variables characteristic of a non-relativistic Maxwell-Boltzmann gas that becomes an isothermal sphere in the Newtonian limit. Consistency criteria lead to a minimal bound for particle masses in the range $30 \hbox{eV} \leq m \leq 60 \hbox{eV}$ and to a constraint between the central temperature and the particles mass. The allowed mass range includes popular supersymmetric particle candidates, such as the neutralino, axino and gravitino, as well as lighter particles ($m\approx$ keV) proposed by numerical N-body simulations associated with self-interactive CDM and WDM structure formation theories.

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