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Spinning planetesimals in a gaseous protoplanetary disk may experience ahydrodynamical force perpendicular to their relative velocities. We examine theeffect this force has on the dynamics of these objects using analyticalarguments based on a simple laminar disk model and numerical integrations ofthe equations of motion for individual grains. We focus in particular onmeter-sized boulders traditionally expected to spiral in to the central star inas little as 100 years from 1 A.U. We find that there are plausible scenariosin which this force extends the lifetime of these solids in the disk by afactor of several. More importantly the velocities induced by the Magnus forcecan prevent the formation of planetesimals via gravitational instability in theinner disk if the size of the dust particles is larger than of order 10 cm. Wefind that the fastest growing linear modes of the streaming instability maystill grow despite the diffusive effect of the Magnus force, but it remains tobe seen how the Magnus force will alter the non-linear evolution of theseinstabilities.

Curveballs in protoplanetary disks - the effect of the Magnus force on planet formation