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Active Region Blinker Intensity Plot

These plots were formed by looking at one particular position on the Sun and plotting the intensity relative to its initial value. The whole event is co-temporal in all lines and lasts from about the 22nd minute to the 27th minute. Just past the 24th minute, the He I intensity peaks at just over twice the initial intensity. The O V plot is even more interesting, showing not only a huge increase in intensity but also clear evidence of a well resolved double peak. This double peak feature is also evident in the hotter WW and Mg IX, although this time the change in intensity peaks at around 20%. Clearly the `active region blinker' can influence the solar atmosphere across a wide range of temperatures.