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We compare the results of the numerical simulation of the viscous-likeinteraction of the solar wind with the plasma tail of a comet, with velocitiesof H2O+ ions in the tail of comet Swift-Tuttle determined by means ofspectroscopic, ground based observations. Our aim is to constrain the value ofthe basic parameters in the viscous-like interaction model: the effectiveReynolds number of the flow and the interspecies coupling timescale. We findthat in our simulations the flow rapidly evolves from an arbitrary initialcondition to a quasi-steady state for which there is a good agreement betweenthe simulated tailward velocity of H2O+ ions and the kinematics derived fromthe observations. The fiducial case of our model, characterized by a loweffective Reynolds number (Re \approx 20 and selected on the basis of acomparison to in situ measurements of the plasma flow at comet Halley, yieldsan excellent fit to the observed kinematics. Given the agreement between modeland observations, with no ad hoc assumptions, we believe that this resultsuggests that viscous-like momentum transport may play an important role in theinteraction of the solar wind and the cometary plasma environment.

Viscous-like Interaction of the Solar Wind with the Plasma Tail of Comet Swift-Tuttle