  X-ray emission from the supermassive star Eta Carinae (\ec) originates from
hot shocked gas produced by current stellar mass loss as well as ejecta from
prior eruptive events. Absorption of this emission by cool material allows the
determination of the spatial and temporal distribution of this material.
Emission from the shocked gas can provide important information about
abundances through the study of thermal X-ray line emission. We discuss how
studies of the X-ray emission from Eta Car at a variety of temporal, spatial
and spectral scales and resolutions have helped refine our knowledge of both
the continuous and discrete mass loss from the system, and its interactions
with more extended material around the star.
