Fine Scale Structure in Cometary Dust Tails - Figure 6.11 - Sunward aligned temporal maps of C/2002 V1 showing tracked striae with and without modelled CME interaction (from C3 Clear images with MGN enhancement)
Sunward aligned temporal maps of C/2002 V1's dust tail as seen by LASCO C3 (clear filter) with MGN enhancement, showing the effects of increased solar wind dynamic pressure of varying strength.
The expected positions of striae under normal Finson Probstein physics have been tracked and are shown in cyan. Their expected positions calculated through enhanced Finson Probstein modelling of CMEs with various multiplier values are shown in magenta.
The CME model only causes significant deviation in expected striae behaviour where the Finson Probstein multiplier is at least one order of magnitude greater than unity.
