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Fine Scale Structure in Cometary Dust Tails - Figure 6.12 - Sunward aligned maps of C/2002 V1 showing how tail morphology (as seen by C3 Clear) changes with a modelled CME interaction
Three sunward aligned maps of C/2002 V1's simulated dust tail position as seen by LASCO C3, showing the effects of increased solar wind dynamic pressure of varying strength.
Dust unaffected by the CME model is shown in blue. Dust which has been dynamically altered by the CME is shown in magenta.
These maps show that a very large Finson-Probstein multiplier is required to cause a significant change in tail morphology.
Interestingly, the model causes dust to collect on the edge of the affected region in the same orientation as a stria.
