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Fig. 7


a) Frequency distribution of background-subtracted LYRA zirconium channel peak irradiance of all non-eclipse-season flares between January 2010 and May 2015 derived with the standard LYRAFF algorithm (start threshold = 1%, first fall threshold = 20%, end threshold = 50%). The distribution above the roll-over does not follow a straight line indicating this distribution is not a power law. b) The same distribution as in a) broken into flares observed by LYRA and GOES/XRS (solid) and those observed by just LYRA (dashed). The flares observed by only LYRA tend to be smaller and have a steeper distribution. c) The same distribution as in a) broken into flares which occurred in 2010 and after 2010. The slope of the 2010 distribution is less steep. We note that the 2010 distribution has been scaled by 25 to make it easier to visually compare its slope with the post 2010 distribution.

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