The effects of main-sequence mass loss on the evolution, interior structure, and surface composition of the sun are studied. Modeling results are presented for three mass-losing solar models of initial mass two solar, plus a standard one solar mass comparison model. It is shown that the solar models can be evolved to produce present-day solar models that do not differ radically in structure and composition from standard solar models. The mass-losing models require low initial He-4 abundances and predict high surface He-3 abundances that are near the limits, yet still within the bounds, of observational estimates. The mass-losing models have somewhat higher B-8 neutrino fluxes, but standard solar models also fail to reproduce observations by a wide margin. For mass-losing models, protosolar Li and Be are completely destroyed, requiring a mechanism for partial replenishment to observed surface abundances. 34 references.