  We compare the hot star wind models calculated assuming older solar abundance
determination with models calculated using the recently published values
derived from 3D hydrodynamical model atmospheres. We show that the use of new
abundances with lower metallicity improves the agreement between wind
observation and theory in several aspects: (1) The predicted wind mass-loss
rates are lower by a factor of 0.76. This leads to a better agreement with
mass-loss rate determinations derived from observations with account of
clumping. (2) As a result of the lowering of mass-loss rates, there is a better
agreement between predicted modified wind momentum-luminosity relationship and
that derived from observations with account of clumping. (3) Both the lower
mass fraction of heavier elements and lower mass-loss rates lead to a decrease
of the opacity in the X-ray region. This has influence on the prediction of the
X-ray line profile shapes. (4) There is a better agreement between predicted PV
ionization fractions and those derived from observations.
