Abstract
Some of the basic effects of particle drifts on cosmic rays in the inner and outer Heliosphere are discussed. We bring arguments supporting that particle drifts, convection and adiabatic cooling can be treated by the same matching condition at discontinuities, the apparent infinite value of drift speed is consistent with the diffusive description. Simple illustrative examples are presented to highlight the differences between drift and no-drift solutions of the Parker equation. A simplistic model simulation is presented to demonstrate the role of drifts in the 22-year solar modulation cycle. The nature and possible effects of drift in the heliosheath are briefly addressed.
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