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We study how halo intrinsic dynamical properties are linked to theirformation processes for halos in two mass ranges, $10^{12}-10^{12.5}h^{-1}{\rmM_\odot}$ and $\ge 10^{13}h^{-1}{\rm M_\odot}$, and how both are correlatedwith the large scale tidal field within which the halos reside at present. Halomerger trees obtained from cosmological $N$-body simulations are used toidentify infall halos that are about to merge with their hosts. We find thatthe tangential component of the infall velocity increases significantly withthe strength of the local tidal field, but no strong correlation is found forthe radial component. These results can be used to explain how the internalvelocity anisotropy and spin of halos depend on environment. The positionvectors and velocities of infall halos are aligned with the principal axes ofthe local tidal field, and the alignment depends on the strength of the tidalfield. Opposite accretion patterns are found in weak and strong tidal fields,in the sense that in a weak field the accretion flow is dominated by radialmotion within the local structure, while a large tangential component ispresent in a strong field. These findings can be used to understand the strongalignments we find between the principal axes of the internal velocityellipsoids of halos and the local tidal field, and their dependence on thestrength of tidal field. They also explain why halo spin increases with thestrength of local tidal field, but only in weak tidal fields does thespin-tidal field alignment follow the prediction of the tidal torque theory. Wediscuss how our results may be used to understand the spins of disk galaxiesand velocity structures of elliptical galaxies and their correlations withlarge-scale structure.

Flow Patterns around Dark Matter Halos: the Link between Halo Dynamical Properties and Large Scale Tidal Field