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The clustering of dark matter haloes with fixed mass depends on theirformation history, an effect known as assembly bias. We use zoom N -bodysimulations to investigate the origin of this phenomenon. For each halo atredshift z=0, we determine the time in which the physical volume containing itsfinal mass becomes stable. We consider five examples for which this happens atz~1.5 and two that do not stabilize by z=0. The zoom simulations show thatearly-collapsing haloes do not grow in mass at z=0 while late-forming ones showa net inflow. The reason is that 'accreting' haloes are located at the nodes ofa network of thin filaments feeding them. Conversely, each 'stalled' halo lieswithin a prominent filament that is thicker than the halo size. Infallingmaterial from the surroundings becomes part of the filament while matter withinit recedes from the halo. We conclude that assembly bias originates fromquenching halo growth due to tidal forces following the formation of non-linearstructures in the cosmic web, as previously conjectured in the literature. Alsothe internal dynamics of the haloes change: the velocity anisotropy profile isbiased towards radial (tangential) orbits in accreting (stalled) haloes. Ourfindings reveal the cause of the yet unexplained dependence of halo clusteringon the anisotropy. Finally, we extend the excursion-set theory to account forthese effects. A simple criterion based on the ellipticity of the linear tidalfield combined with the spherical collapse model provides excellent predictionsfor both classes of haloes.

ZOMG-I. How the cosmic web inhibits halo growth and generates assembly bias