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A comet ionospheric model assuming the plasma to move radially outward withthe same bulk speed as the neutral gas and not being subject to severereduction through dissociative recombination has previously been tested in aseries of case studies associated with the Rosetta mission at comet67P/Churyumov-Gerasimenko. It has been found that at low activity and withinseveral tens of km from the nucleus such models (which originally weredeveloped for such conditions) generally work well in reproducing observedelectron number densities, in particular when plasma production through bothphotoionization and electron-impact ionization is taken into account. Nearperihelion, case studies have, on the contrary, showed that applying similarassumptions overestimates the observed electron number densities at thelocation of Rosetta. Here we compare ROSINA/COPS driven model results withRPC/MIP derived electron number densities for an extended time period (2015November through 2016 March) during the post-perihelion phase with southernsummer/spring. We observe a gradual transition from a state when the modelgrossly overestimates (by more than a factor of 10) the observations to beingin reasonable agreement during 2016 March.

The evolution of the electron number density in the coma of comet 67P at the location of Rosetta from 2015 November through 2016 March