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Fig. 7.

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Modelled X-ray fluxes (plus signs) compared to GOES (top panel), and to RHESSI 6–10 keV (bottom panel). Obtained values are slightly lower than the GOES flux as we modelled only the emission coming from the fraction of the solar surface. The agreement between the model and RHESSI fluxes is the method constraint – we were changing the cut-off energy until agreement was achieved.

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