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The orbital decay of a perturber within a larger system plays a key role inthe dynamics of many astrophysical systems -- from nuclear star clusters orglobular clusters in galaxies, to massive black holes in galactic nuclei, todwarf galaxy satellites within the dark matter halos of more massive galaxies.For many decades, there have been various attempts to determine the underlyingphysics and time-scales of the drag mechanism, ranging from the local dynamicalfriction approach to descriptions based on the back-reaction of global modesinduced in the background system. We present ultra-high-resolution $N$-bodysimulations of massive satellites orbiting a Milky Way-like galaxy (with $>10^8$ particles), that appear to capture both the local "wake" and the global"mode" induced in the primary halo. We address directly the mechanism oforbital decay from the combined action of local and global perturbations andspecifically analyze where the bulk of the torque originates.

Revisiting dynamical friction: the role of global modes and local wakes