Stars are the birth places of the chemical elements in the Universe, and their extensive mass loss provides an important source of gas and dust to the interstellar medium. An understanding of the late phases of stellar evolution, the nature of the mass loss process itself, and the properties of the mass eject are important inputs for studies of the chemical evolution of a galaxy and the formation and evolution of subsequent generations of stars. The nuclear fusion in the stellar interiors of intermediate mass stars create carbon, nitrogen, and oxygen. During the late stage of stellar evolution known as the asymptotic giant branch (AGB), such stars undergo a series of violent mass ejections. The existence of this processed circumstellar material provides a historical record of this evolution. In this talk, I will describe the structure of this material as probed by instruments/telescopes characterized by high sensitivity, spatial resolution and wide wavelength coverage and how their diverse morphology can be theoretically explained in terms of gravitational and hydrodynamical effects in a model for AGB stars in binary systems.