Authors: Maria D. Kazachenko (University of Colorado Boulder / National Solar Observatory), Yuhong Fan (High Altitude Observatory), Andrei Afanasev (University of Colorado Boulder / National Solar Observatory)

Violent solar flares and coronal mass ejections (CMEs) are magnetic phenomena. Advances in observational techniques have allowed us to derive statistical properties of observed flare ribbons, coronal dimmings and magnetic field changes and use them to constrain magnetic field properties of 3D eruptive phenomena (see review by Kazachenko et al. 2022). However these studies focus on observed proxies of hard-to-observe coronal magnetic fields using coronal/chromospheric emission and/or photospheric magnetic field maps, rather than the coronal field directly. Here we complement existing knowledge of these observed proxies by performing an in-depth analysis of simulation data from a data-driven magnetohydrodynamic simulation of the 2011-02-15 CME event in active region 11158. We analyze the evolution of ribbon and dimming proxies and compare them with 3D magnetic field evolution during the eruption. We discuss how observed dimming and ribbon properties could help us constrain realistic magnetic field evolution during solar eruptions and discuss their limitations.