Fig. C.1.
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Response functions of (a) HRIEUV, four EUV channels of AIA and (b) and contribution functions of five emission lines measured by SPICE, computed with CHIANTI V 10.1. The abundance is set to ones estimated in the corona by Asplund et al. (2021) and the ionization equilibrium is the one recommended by CHIANTI. Here, the density is fixed to ne = 1 × 109 cm−3.
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