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Properties of the solar wind are discussed and applied to the effect of thewind on motion of bodies in the Solar System. The velocity density function forthe solar wind constituents is given by the $\kappa-$distribution. The relevantcontributions to the solar wind action contain also the sputtering andreflection components in addition to direct impact. The solar wind effect ismore important than the action of the solar electromagnetic radiation, as forthe secular orbital evolution. The effect of the solar corpuscular radiation ismore important than the Poynting-Robertson effect even when mass of the dustparticle is considered to be constant, non-radial component of the solar windvelocity is neglected and the time dependence of the solar wind properties isignored.  The presented equation of motion of a body under the action of the solarradiation, electromagnetic and corpuscular, respects reality in a much betterway than the conventionally used equation. The acceleration of the body isproportional to the superposition of the radial velocity component multipliedby the numerical coefficient $[2 + (\eta_{1} + \eta_{2})/ \overline{Q}~'_{pr}]$ and the transversal velocity component multiplied by the numericalcoefficient $(1 + \eta_{2}/ \overline{Q} ~'_{pr})$, where $\overline{Q}~'_{pr}$ is the dimensionless efficiency factor of the radiation pressure. Here$\eta_{1}$ $\doteq$ 1.1, $\eta_{2}$ $\doteq$ 1.4 and the velocity is the body'svelocity with respect to the Sun. Also time variability of $\eta_{1}$ and$\eta_{2}$ due to the solar cycle is given.  The dimensionless cross section the dust grain presents to wind pressure isabout 4.7. This value differs from the conventionally used value 1.0. Themass-loss rate of the zodiacal cloud is 4-times higher than the currentlyaccepted value, as for the micron-sized dust particles.

Solar wind dominance over the Poynting-Robertson effect in secular orbital evolution of dust particles