  Apparent excesses in early-solar $^{26}$Al, $^{36}$Cl, $^{41}$Ca, and
$^{60}$Fe disappear if one accounts for ejecta from massive-star winds
concentrated into dense phases of the ISM in star-forming regions. The removal
of apparent excesses is evident when wind yields from Wolf-Rayet stars are
included in the plot of radionuclide abundances vs. mean life. The resulting
trend indicates that the solar radionuclides were inherited from parental
molecular clouds with a characteristic residence time of 10$^8$ years. This
residence time is of the same order as the present-day timescale for conversion
of molecular cloud material into stars. The concentrations of these extinct
isotopes in the early solar system need not signify injection from unusual
proximal stellar sources, but instead are well explained by normal
concentrations in average star-forming clouds. The results imply that the
efficiency of capture is greater for stellar winds than for supernova ejecta
proximal to star-forming regions.
