Comparative characterization of mass-loss vs. obscuration dimming

Compare and characterize coronal mass-loss dimming and obscuration dimming in relation to coronal mass ejections (CMEs) by determining how each signature correlates with CME mass, speed, geometry, and line-of-sight orientation in spatially resolved solar data and Sun-as-a-star or stellar observations.

Background

Coronal dimmings arise via different mechanisms: mass-loss dimming from evacuated coronal plasma during CMEs, and obscuration dimming from absorption by cool, optically thick eruptive material (e.g., filaments).

A rigorous comparative framework would enhance CME detection and parameter estimation in unresolved stellar data and improve the reliability of CME proxies used for exospace weather studies.