  The assembly and architecture of planetary systems strongly depend on the
physical processes governing the evolution and dispersal of protoplanetary
disks. Since Protostars and Planets VI, new observations and theoretical
insights favor disk winds as being one of those key processes. This chapter
provides a comprehensive review of recent observations probing outflowing gas
launched over a range of disk radii for a wide range of evolutionary stages,
enabling an empirical understanding of how winds evolve. In parallel, we review
theoretical advancements in both magnetohydrodynamic and photoevaporative disk
wind models and identify predictions that can be confronted with observations.
By linking theory and observations we critically assess the role of disk winds
in the evolution and dispersal of protoplanetary disks. Finally, we explore the
impact of disk winds on planet formation and evolution and highlight
theoretical work, observations, and critical tests for future progress.
