http://arxiv.org/abs/1703.02995
Extreme Ultraviolet (EUV) solar flare emissions evolve in time as the emitting plasma heats and then cools. Although accurately modeling this evolution has been historically difficult, especially for empirical relationships, it is important for understanding processes at the Sun, as well as for their influence on planetary atmospheres. With a goal to improve empirical flare models, a new simple empirical expression has been derived to predict how cool emissions will evolve based on the evolution of a hotter emission. This technique was initially developed by studying 12 flares in detail observed by the EUV Variability Experiment (EVE) onboard the Solar Dynamics Observatory (SDO). Then, over 1100 flares observed by EVE were analyzed to validate these relationships. These results have practical implications in improving flare irradiance modeling and for identifying key emission lines for future monitoring of flares for space weather operations, and also provide insight into the cooling processes of flare plasma.
E. Thiemann, F. Eparvier and T. Woods
Fri, 10 Mar 17
51/52
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