The Structure and Dynamics of Massive High-$z$ Cosmic-Web Filaments: Three Radial Zones in Filament Cross-Sections

We analyse the internal structure and dynamics of cosmic-web filaments that connect massive high-$z$ haloes. Our analysis is based on a high-resolution AREPO cosmological simulation zooming-in on a volume encompassing three $\mathrm{M}\mathrm{p}\mathrm{c}$-scale filaments feeding three massive haloes of $\sim {10}^{12}{\text{M}}_{\odot }$ at $z\sim 4$, embedded in a large-scale sheet. Each filament is surrounded by a cylindrical accretion shock of radius $r_{\mathrm{s}\mathrm{h}\mathrm{o}\mathrm{c}\mathrm{k}}\sim 50\mathrm{k}\mathrm{p}\mathrm{c}$. The post-shock gas is in virial equilibrium with the potential well set by an isothermal dark-matter filament. The filament line-mass is $\sim 9\times {10}^8{\text{M}}_{\odot }{\mathrm{k}\mathrm{p}\mathrm{c}}^{-1}$, the gas fraction within $r_{\mathrm{s}\mathrm{h}\mathrm{o}\mathrm{c}\mathrm{k}}$ is the universal baryon fraction, and the virial temperature is $\sim 7\times {10}^5\mathrm{K}$. In the outer ‘‘thermal’’ (T) zone, $r\ge 0.65r_{\mathrm{s}\mathrm{h}\mathrm{o}\mathrm{c}\mathrm{k}}$, inward gravity and ram-pressure forces are over-balanced by outwards thermal pressure forces, decelerating the inflowing gas expanding the shock outward. In the intermediate ‘‘vortex’’ (V) zone, $0.25\le r\mathrm{/}{r}_{\mathrm{s}\mathrm{h}\mathrm{o}\mathrm{c}\mathrm{k}}\le 0.65$, the velocity field is dominated by a quadrupolar vortex structure due to offset inflow along the sheet through the post-shock gas. The outwards force is dominated by centrifugal forces associated with these vortices, with additional contributions from global rotation and thermal pressure. The shear and turbulent forces associated with the vortices act inward. The inner ‘‘stream’’ (S) zone, $r<0.25r_{\mathrm{s}\mathrm{h}\mathrm{o}\mathrm{c}\mathrm{k}}$, is a dense isothermal core, $T\sim 3\times {10}^4\mathrm{K}$ and $n_{\mathrm{H}}\sim 0.01\mathrm{c}{\mathrm{m}}^{-3}$, defining the cold streams that feed galaxies. The core is formed by an isobaric cooling flow and is associated with a decrease in outwards forces, though it exhibits both inflows and outflows. [abridged]