📝 SummarXiv

Abstract

We study dark matter halos modeled by general relativistic polytropic spheres in spacetimes with the repulsive cosmological constant representing vacuum energy density, governed by a polytropic index $n$ and a relativistic (cosmological) parameter $\sigma$ ($\lambda$) determining the ratio of central pressure (vacuum energy density) and central energy density of the fluid. To give mapping of the polytrope parameters for matching extension and mass of large dark matter halos, we study properties of the polytropic spheres and introduce an effective potential of the geodesic motion in their internal spacetime. Circular geodesics enable us to find the limits of the trapping polytropes with central regions containing trapped null geodesics; supermassive black holes can be formed due to the instability of the central region against gravitational perturbations. Stability of the polytropic spheres relative to radial perturbations is determined. We match extension and mass of the polytropes to those of dark matter halos related to large galaxies or galaxy clusters, with extension $100 < \ell/\mathrm{kpc} < 5000$ and gravitational mass $10^{12} < M/M_\odot < 5 \times 10^{15}$. The observed velocity profiles simulated by the phenomenological dark matter halo density profiles can be well matched also by the velocity profiles of the exact polytrope spacetimes. The matching is possible by the non-relativistic polytropes for each value of $n$, with relativistic parameter $\sigma \leq 10^{-4}$ and very low central energy density. Surprisingly, the matching works for ``spread'' relativistic polytropes with $n > 3.3$ and $\sigma \geq 0.1$ when the central density can be much larger. The trapping polytropes forming supermassive black holes must have $n > 3.8$ and $\sigma > 0.667$.