While gradient and curvature drifts are well-established elements of
the propagation of cosmic rays in the heliospheric magnetic field,
their perturbation by the Solar activity-induced large-scale
distortions of dipole-like field configurations even during Solar
minima and by magnetic turbulence is an open problem. Various
empirical or phenomenological approaches have been suggested to
quantify these effects so that they can be straightforwardly
incorporated in modulation models covering the 22-year periodicity
(including the sign) of Solar activity. These approaches, however,
either lack clear physics-based parametrizations (e.g., in terms of
the tilt-angle of the heliospheric current sheet) or have been shown
to be incompatible with measurements (like a dependence on the
normalized turbulence level). We propose here a new
approach to the treatment of drifts over an entire Solar cycle
including maximum periods, which is based on Solar magnetograms. This
not only provides a physics-based approach to the reduction of drifts
during Solar activity maxima but also a treatment that is fully
consistent with those MHD models of the Solar wind and the embedded
heliospheric magnetic field that exploit Solar magnetograms as inner
boundary conditions.