Solar wind charge exchange in cometary atmospheres: III. Results from the Rosetta mission to comet 67P/Churyumov-Gerasimenko (vol 630, A37, 2019)

The original article shows figures with incorrect column densities (Fig. 3A), outgassing rates from the ROSINA-COPS instrument (Fig. 5A, black line and Fig. 6, black line), and energetic neutral atom (ENA) predictions (Figs. 9 and 10). These are all corrected below; their unchanged caption is given here for convenience. Because this mistake was only made for figures, the results and conclusions of the original article remain unchanged except for the following sentences: Section 4.4, p. 12. Regarding Fig. 9, pertaining to the helium species and the importance of ENAs, the sentence should read: “In extremely rare events, we predict that ENAs could reach 50% of the He2+ signal and dominate over He+ ions: this may have occurred once on 24 April 2015 and after perihelion on 12 and 31 December 2015 as well as on 6-7 February 2016.” Correspondingly, when discussing the hydrogen species in the next paragraph, the dates should be amended so that: “the ENA flux may even become higher than the proton flux in very rare events (ratio above 1, as in February and March 2015, and after perihelion in December 2015, occasionally in January and February 2016, and large periods of time in March and May 2016). The highest predicted ENA fluxes are immediately after Rosetta exited the solar wind ion cavity (SWIC).” Section 4.4, p. 13. Regarding Fig. 10, the predicted dates for a favorable detection of H should be changed and the sentence should read as follows: “Our model predicts the most favorable detection conditions for H in December 2015, around mid-March 2016, and in May 2016”.