Abstract
There are two major effects of mass loss from stars of intermediate mass. First, the ultimate fate of such stars--whether they become supernovae of the type that leave no condensed remnant or whether they become white dwarfs--is extremely sensitive to the rate at which they lose mass during the last portion of their nuclear-burning lives. Second, the contribution of intermediate-mass stars to the enrichment of the interstellar medium in helium, carbon, nitrogen, s-process isotopes, and possibly also in iron-peak elements and r-process isotopes is similarly sensitive to mass-loss rates during this last, quiet phase of nuclear burning.
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