By analyzing resolved solar observations, we reveal significant temporal evolution in white-light flare area and temperature. Based on these findings, our new energy estimation method systematically yields lower flare energies, prompting a re-examination of classical macroscopic scaling laws.
A strong limb flare observed simultaneously by the SDO/AIA and SDO/HMI, which is very rare, allows the authors to study the emission mechanism for white-light flare loops, as well as estimate the electron densities along the flare loop.
What makes the limb flares detectable in visible lights, hydrogen recombination or Thomson scattering?
By synthesizing the results of photospheric field change indicated by HMI observations and coronal field variation suggested by the NLFFF modeling, we study the flare-related 3D magnetic restructuring and find it consistent with the coronal implosion scenario in the low solar atmosphere.