Stars die by mass loss. During their final phase of nuclear burning, while on the Asymptotic Giant Branch, between 20% and 80% of the mass of the star is ejected, causing the transition from star to white dwaf and, briefly, the emergence of a planetary nebula. This superwind determines the white dwarf mass distribution, and is the origin of up to half of the gas and dust in the ISM. The cause,of this catastrophic mass loss is still a matter of debate. This talk will discuss the role of dust in driving the mass loss. The influence of binarity on the winds will be discussed, leading to Hubble winds. Finally, the binary stellar population of the Galactic Bulge will be discussed.