  Intense mass loss through cool, low-velocity winds is a defining
characteristic of low-to-intermediate mass stars during the asymptotic giant
branch (AGB) evolutionary stage. Such winds return up ~80% of the initial
stellar mass to the interstellar medium and play a major role in enriching it
with dust and heavy elements. A challenge to understanding the physics
underlying AGB mass loss is its dependence on an interplay between complex and
highly dynamic processes, including pulsations, convective flows, shocks,
magnetic fields, and opacity changes resulting from dust and molecule
formation. I highlight some examples of recent advances in our understanding of
late-stage stellar mass loss that are emerging from radio and (sub)millimeter
observations, with a particular focus on those that resolve the surfaces and
extended atmospheres of evolved stars in space, time, and frequency.
