  We investigate the combined effect of solar wind, Poynting-Robertson drag,
and the frozen-in interplanetary magnetic field on the motion of charged dust
grains in our solar system. For this reason we derive a secular theory of
motion by the means of averaging method and validate it with numerical
simulations of the un-averaged equations of motions. The theory predicts that
the secular motion of charged particles is mainly affected by the z-component
of the solar magnetic axis, or the normal component of the interplanetary
magnetic field. The normal component of the interplanetary magnetic field leads
to an increase or decrease of semi-major axis depending on its functional form
and sign of charge of the dust grain. It is generally accepted that the
combined effects of solar wind and photon absorption and re-emmision
(Poynting-Robertson drag) lead to a decrease in semi-major axis on secular time
scales. On the contrary, we demonstrate that the interplanetary magnetic field
may counteract these drag forces under certain circumstances. We derive a
simple relation between the parameters of the magnetic field, the physical
properties of the dust grain as well as the shape and orientation of the
orbital ellipse of the particle, which is a necessary conditions for the
stabilization in semi-major axis.
