The impact of the dark matter-gas interaction on the collapse behaviour of spherical symmetric systems

TL;DR

This paper explores how the interaction between dark matter and gas during halo collapse influences the dynamics and evolution, highlighting the importance of backreaction effects in spherical symmetric systems.

Contribution

It introduces a fluid approximation for dark matter with adiabatic contraction and investigates the backreaction effects on halo collapse dynamics.

Findings

Dynamical interaction can shorten collapse times.

System behavior depends on initial density profile shape.

Interaction effects are significant for certain halo mass ranges.

Abstract

If the gas in the evolving cosmic halos is dissipating energy (cooling) then due to the variation of the gravitational potential the dark matter halo also undergoes a compactification. This is well-known as Adiabatic contraction (AC). Complementary to the AC we investigate the resulting dynamical behaviour of the whole system if the backreaction of the AC of DM onto the gas is taken into account. In order to achieve sufficient high resolution also within the central halo region, we use a crude fluid approximation for the DM obeying the adiabatic contraction behaviour. Further, we restrict ourself to spherical symmetry and vanishing angular momentum of the studied matter configurations. The computations are done using a first-order Godunov type scheme. Our results show that the dynamical interaction between gas and DM may lead to significant shorter collapse times. If the gas cools the dynamical behaviour of the whole system depends strongly on the shape of the initial density profile. Our findings indicate that for a certain mass range of halo configurations the dynamical interaction between gas and DM might be important for the halo evolution and must be taken into account.