Polytropic dark matter flows illuminate dark energy and accelerated expansion

TL;DR

This paper proposes a polytropic dark matter fluid model that explains the universe's accelerated expansion and dark energy phenomena without requiring a separate dark energy component, fitting observational data well.

Contribution

It introduces a single-parameter polytropic dark matter model that accounts for cosmic acceleration and fits supernova data, challenging traditional dark energy theories.

Findings

The model explains cosmic acceleration without dark energy.

It fits supernova distance measurements accurately.

The model avoids age and coincidence problems.

Abstract

Currently, a large amount of data implies that the matter constituents of the cosmological dark sector might be collisional. An attractive feature of such a possibility is that, it can reconcile dark matter (DM) and dark energy (DE) in terms of a single component, accommodated in the context of a polytropic-DM fluid. Accordingly, we explore the time evolution and the dynamical characteristics of a spatially-flat cosmological model, in which, in principle, there is no DE at all. Instead, in this model, the DM itself possesses some sort of fluid-like properties, i.e., the fundamental units of the Universe matter-energy content are the volume elements of a DM fluid, performing polytropic flows. In this case, the energy of this fluid's internal motions is also taken into account as a source of the universal gravitational field. This form of energy can compensate for the extra energy needed to compromise spatial flatness, namely, to justify that, today, the total-energy density parameter is exactly unity. The polytropic cosmological model, depends on only one free parameter, the corresponding exponent, \Gamma. What makes this model particularly interesting, is that, for \Gamma < 0.541, the (conventional) pressure becomes negative enough, so that the Universe accelerates its expansion at cosmological redshifts below a transition value. Several physical reasons impose further constraints on the value of \Gamma, which, eventually, is settled down to the range -0.089 < \Gamma < 0. Such a cosmological model does not suffer either from the age problem or from the coincidence problem. At the same time, this model reproduces to high accuracy the distance measurements performed with the aid of the supernovae Type Ia standard candles, and most naturally interprets, not only when, but also, why the Universe transits from deceleration to acceleration, thus arising as a mighty contestant for a DE model.