Quasi-spiral solution to the mixed intracluster medium and the universal entropy profile of galaxy clusters

TL;DR

This paper proposes a quasi-spiral hydrodynamic solution for the intracluster medium in galaxy clusters, explaining observed structures and entropy profiles through self-similar spiral formations influenced by gravitational potential and plasma mixing.

Contribution

It introduces a novel quasi-stationary spiral model for the ICM that accounts for observed entropy profiles and large-scale structures in galaxy clusters, supported by simulations.

Findings

Spiral structures naturally form in simulated ICM with angular momentum and mixing.

The spiral solution explains the universal entropy profile $K(r) \\propto r$.

Spirals can be sustained by outflows and buoyant plasma phases.

Abstract

Well-resolved galaxy clusters often show a large-scale quasi-spiral structure in deprojected density $\rho$ and temperature $T$ fields, delineated by a tangential discontinuity known as a cold front, superimposed on a universal radial entropy profile with a linear $K(r)\propto T\rho^{-2/3}\propto r$ adiabat. We show that a spiral structure provides a natural quasi-stationary solution for the mixed intracluster medium (ICM), introducing a modest pressure spiral that confines the locally buoyant or heavy plasma phases. The solution persists in the presence of uniform or differential rotation, and can accommodate both an inflow and an outflow. Hydrodynamic adiabatic simulations with perturbations that deposit angular momentum and mix the plasma thus asymptote to a self-similar spiral structure. We find similar spirals in Eulerian and Lagrangian simulations of 2D and 3D, merger and offset, clusters. The discontinuity surface is given in spherical coordinates $\{r,\theta,\phi\}$ by $\phi(r,\theta)\propto \Phi(r)$, where $\Phi$ is the gravitational potential, combining a trailing spiral in the equatorial ($\theta=\pi/2$) plane and semicircles perpendicular to the plane, in resemblance of a snail shell. A local convective instability can develop between spiral windings, driving a modified global instability in sublinear $K(r)$ regions; evolved spirals thus imprint the observed $K\propto r$ onto the ICM even after they dissipate. The spiral structure brings hot and cold phases to close proximity, suggesting that the observed fast outflows could sustain the structure even in the presence of radiative cooling.