oronal Mass Ejections and Dimmings: A Comparative Study using MHD Simulations and SDO Observations

Solar coronal dimmings have been observed extensively in the past twodecades. Due to their close association with coronal mass ejections (CMEs),there is a critical need to improve our understanding of the physical processesthat cause dimmings as well as their relationship with CMEs. In this study, weinvestigate coronal dimmings by combining simulation and observational efforts.By utilizing a data-constrained global magnetohydrodynamics model (AWSoM:Alfven-wave Solar Model), we simulate coronal dimmings resulting from differentCME energetics and flux rope configurations. We synthesize the emissions ofdifferent EUV spectral bands/lines and compare with SDO/AIA and EVEobservations. A detailed analysis of the simulation and observation datasuggests that the transient dimming / brightening are related to plasma heatingprocesses, while the long-lasting core and remote dimmings are caused by massloss process induced by the CME. Moreover, the interaction between the eruptingflux rope with different orientations and the global solar corona couldsignificantly influence the coronal dimming patterns. Using metrics such asdimming depth and dimming slope, we investigate the relationship betweendimmings and CME properties (e.g., CME mass, CME speed) in the simulation. Ourresult suggests that coronal dimmings encode important information about theassociated CMEs, which provides a physical basis for detecting stellar CMEsfrom distant solar-like stars.