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Fig. 10.


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Variation with wavelength of the difference of intensity between flare and preflare times in three wavelength ranges containing continuum regions (dw1 and dw2) and the Mg II h & k line. The differences in intensity have been multiplied by the transmission filter profile f(λ) of the 2832 Å filter (Kleint et al. 2017). After normalization of the hatched areas in panelsb and c, we estimate that the contribution of the excess of the Balmer emission is 82% compared to the contribution of the Mg II k line around 18% in the wavelength domain of the 2832 Å SJI during the flare.

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