Observed Diffusive Emission from the Solar Corona and Role of Endogenous Magnetic Reconnection

Considering the hot solar coronal loops observed by the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO), the X-ray telescope (XRT) and the Extreme Ultraviolet Imaging Spectrometer (EIS) on Hinode, we propose a possible explanation for the heating of Corona and the generation of high energy particle populations that may be responsible for the observed Diffusive Emission. Diffusive Emission is a form of X-ray coronal emission not confined within observationally distinct coronal loops. The relevant theoretical model is based on an endogenous reconnection process [1] that is sustained by the electron temperature gradient inside the reconnection layer, when the evolving electron temperature fluctuations are not isotropic. The inputs for this model are obtained from the most recent observations of AIA, XRT and EIS.

[1] B. Coppi and B. Basu, Phys. Lett. A, 382, 400 (2018).