image: Solar cycle changes in the solar corona as viewed by Atmospheric Imaging Assembly (AIA) on the Solar Dynamic Observatory in extreme ultraviolet (EUV) toward the end of the latest solar minimum activity period in May 2010 (left half) and during the current solar maximum period in December 2014 (right half). The three-color red, green and blue image channels are composed of observations made in three AIA channels: 171, 193, and 211 Å, respectively, corresponding to their most dominant emission lines of Fe IX, Fe XII, and Fe XIV with formation temperatures of ~0.7, 1.2, and 2.0 MK. This material relates to a paper that appeared in the July 14, 2017, issue of Science Advances, published by AAAS. The paper, by H. Morgan at Aberystwyth University in Aberystwyth, UK, and colleagues was titled, 'Global conditions in the solar corona from 2010 to 2017.' view more
Credit: [Credit: Morgan <i>et al.</i> Sci. Adv. 2017;3: e1602056]