  The initial conditions, physics, and outcome of planet formation are now
constrained by detailed observations of protoplanetary disks, laboratory
experiments, and the discovery of thousands of extrasolar planetary systems.
These developments have broadened the range of processes that are considered
important in planet formation, to include disk turbulence, radial drift, planet
migration, and pervasive post-formation dynamical evolution. The N-body
collisional growth of planetesimals and protoplanets, and the physics of
planetary envelopes - key ingredients of the classical model - remain central.
I provide an overview of the current status of planet formation theory, and
discuss how it connects to observations.
