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.