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We use high-resolution zoom-in simulations to study the fueling of thecentral galaxies by gas accretion from cosmological filaments at highredshifts, z>=2. Their parent haloes with similar DM masses oflog(M_vir/M})~11.65, have been chosen at z=6, 4, and 2, in high/low overdensityenvironments, with the goal of comparing evolution within similar M atdifferent z, under dual action of cosmological accretion and galactic outflows-- forming the circumgalactic medium (CGM). We focus on the filamentary anddiffuse gas accretion within few virial radii, R_vir, down to the centralgalaxy. Using a hybrid d-web/entropy method we have mapped the gaseousfilaments, and invoking particle kinematics allowed us to separate inflows fromoutflows, thus resolving thermodynamic and kinematic signatures of the CGM. Wefind that (1) The CGM is multiphase and not in thermodynamic or dynamicequilibrium; (2) accretion rates via individual filaments display a loweraccretion rate and densities at lower redshifts. The inflow velocities alongthe filaments decrease with redshift, z~ 6-2, from 200-30 kms^-1 by a factor of2; (3) Temperature within the filaments increases inside R_vir, faster at lowerredshifts, in tandem with decrease in the accretion rate; (4) The filamentsshow a complex structure along their spines: a core radial flow surrounded by alower density envelope. The core exhibits an elevated density and lowertemperature, with no obvious metallicity gradient in the filament crosssections. It also tends to separate the filament into different infall velocityregions and density cores, thus producing a spaghetti-type flow; (6) Inside theinner ~ 30\,h^-1 kpc, the filaments develop the Kelvin-Helmholtz instabilitywhich ablates and dissolves them, and triggers turbulence along the filamentspine; (7) Finally, the galactic outflows affect mostly the inner ~ 0.5R_vir~100 h^-1 kpc of the CGM.

Dissecting Cosmological Filaments at High Redshifts: Emergence of Spaghetti-type Flow Inside DM Haloes