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(Abridged) We perform dissipationless N-body simulations to elucidate thedynamical response of thin disks to bombardment by cold dark matter (CDM)substructure. Our method combines (1) cosmological simulations of the formationof Milky Way (MW)-sized CDM halos to derive the properties of substructure and(2) controlled numerical experiments of consecutive subhalo impacts onto aninitially-thin, fully-formed MW type disk galaxy. The present study is thefirst to account for the evolution of satellite populations over cosmic time insuch an investigation of disk structure. We find that accretions of massivesubhalos onto the central regions of host halos, where the galactic disksreside, since z~1 should be common. One host halo accretion history is used toinitialize the controlled simulations of satellite-disk encounters. We showthat these accretion events severely perturb the thin galactic disk and producea wealth of distinctive dynamical signatures on its structure and kinematics.These include (1) considerable thickening and heating at all radii, with thedisk thickness and velocity ellipsoid nearly doubling at the solar radius; (2)prominent flaring associated with an increase in disk thickness greater than afactor of 4 in the disk outskirts; (3) surface density excesses at large radii,beyond ~5 disk scale lengths, resembling those of observed antitruncated disks;(4) lopsidedness at levels similar to those measured in observational samplesof disk galaxies; and (5) substantial tilting. The interaction with the mostmassive subhalo drives the disk response while subsequent bombardment is muchless efficient at disturbing the disk. We conclude that substructure-diskencounters of the kind expected in the LCDM paradigm play a significant role insetting the structure of disk galaxies and driving galaxy evolution.

Cold Dark Matter Substructure and Galactic Disks II: Dynamical Effects of Hierarchical Satellite Accretion