We have computed detailed solar models, taking early-main-sequence mass loss into account. We have followed the nuclear destruction (and production) of Li-7 throughout the interior structure of the star during the entire evolution, keeping careful account of the changes in the surface lithium abundance due to mass loss and convection. We have considered initial masses of M(i) = 1.8, 1.5, 1.2, and 1.1 M., each with mass-loss time scales of tau-m = 0. 16, 0.5, and 0.985 Gyr. A solar model of initial mass M(i) almost-equal-to 1.1 M. can solve the case of the missing solar lithium, producing the observed surface lithium depletion of a factor of 100. Furthermore, this lithium depletion is almost independent of the mass-loss time scale. With this mass loss of only DELTA-M almost-equal-to 0.1 M., there are only minor changes in the presolar helium abundance, the solar metallicity, the mixing-length parameter, and the predicted solar neutrino capture rates. We estimate that this mass loss would cause the convective envelope to just reach the layers where Be-9 has been burned, resulting in little surface Be-9 depletion, in agreement with solar observations. The higher initial masses are ruled out unless there is some mechanism to produce Li-7 (and Be-9) at the solar surface. Main-sequence mass loss reduces the required presolar helium abundance (which must always exceed the primordial abundance); this constrains the mass loss DELTA-M to be less than 0.7, 1.0, and 1.5-2 M. for mass-loss time scales tau-m = 0.985, 0.5, and 0.16 Gyr, respectively (a much weaker constraint than that obtained from Li-7 depletion). For mass-losing cases, Li-7 and Be-9 burning does not take place at usually assumed temperatures of 2.5 x 10(6) and 3.3 x 10(6) K, respectively, but requires higher initial temperatures of approximately 3 x 10(6) and 4 x 10(6) K, respectively. The difference is due to the decline of these temperatures caused by the mass loss. We have developed a simple prescription to estimate these initial temperatures for Li-7 and Be-9 burning in mass-losing cases. The luminosity history of our M(i) = 1.1 M. case is different from that of the standard solar model, with an initial decline during the mass-loss period (rather than a steady brightening) but with smaller total variation. This, together with the larger initial gravity and larger initial solar wind [M(i) = (1-7) x 10(-10) M. yr-1], would have had a significant effect on the solar planetary system, which should be explored further.
