  The possibility that the chemical composition of the solar atmosphere has
been affected by radiative dust cleansing of late and weak accretion flows by
the proto-sun itself, is explored. Estimates, using semi-analytical methods and
numerical simulations of the motion of dust grains in a collapsing non-magnetic
and non-rotating gas sphere with a central light source are made, to model
possible dust-cleansing effects. Our calculations indicate that the amounts of
cleansed material may well be consistent with the abundance differences
observed for the Sun when compared with solar-like stars and with the relations
found between these differences and condensation temperature of the element. It
seems quite possible that the proposed mechanism might have produced the
significant abundance effects observed for the Sun, provided that late and
relatively weak accretion did occur. The effects of cleansing may, however, be
affected by outflows from the Sun, the existence and dynamics of magnetic
fields and of the accretion disk, and the possible presence and location of the
Early Sun in a rich stellar cluster.
