Modeling the Excitation, Propagation, and Damping of Quasiperiodic Fast Magnetosonic Waves in Realistic Coronal Active Region Magnetic Field Structures

Abstract Quasiperiodic fast propagating (QFP) magnetosonic waves have been discovered in the solar corona in the extreme ultraviolet (EUV) since the launch of the Solar Dynamics Observatory (SDO) spacecraft more than a decade ago. The QFP waves are associated with flares and coronal mass ejections, providing information on flare pulsations as well as on the magnetic field by MHD wave seismology. Previous models of QFP waves primarily used idealized magnetic active region (AR) structures. However, more realistic AR numerical models are needed to improve the application of coronal seismology to observations of waves in coronal structures. Here, we extend the previous models by including a realistic magnetic configuration based on an observed coronal AR in a case study using AR 11166, observed on 2011 March 10 by the SDO Atmospheric Imaging Assembly, using potential field extrapolation of the photospheric magnetic field with realistic gravitationally stratified density structure and typical coronal temperature in our resistive 3D MHD model. We aim at reproducing the observed QFP properties, such as directionality, propagation, reflection, nonlinearity, and damping of these waves. We model various forms of excitation of QFPs through time-dependent boundary conditions and localized pulses at the base of the corona. We produce synthetic emission measure maps from the 3D MHD modeling results to facilitate comparison to EUV observations. We find that the present, more realistic model provides better qualitative agreement with observations compared to previous idealized models, improving the study of QFP wave excitation, propagation, and damping in coronal ARs, with potential applications to coronal seismology.