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Fig. 7.


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Same as Figures 2 and 6 but considering a longer time range. We have included the simulated profiles obtained with our closest model (shown in amber) while a model in which the post-eruption solar wind was slower down to  km s−1 (in red). It results in a better fit of the rarefaction zone. The in situ data obtained by WIND are shown in black lines with a smooth window of 15 min.

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