Solar wind flux reconstructed from the inversion of the analytical model compared to the original input solar wind upstream flux (Slavin & Holzer 1981) during the Rosetta mission (2014–2016). Proton and α particle fluxes (4% of the total solar wind ions) are considered. Dotted lines are results of the forward analytical model with a solar wind Maxwellian temperature T = 40 × 10⁶ K. Otherwise, the caption is the same as for Fig. 7.