The Role of Photospheric Magnetic Field Variations in Sunquake Generation

Sunquakes are seismic waves observed on the Sun's photosphere connected to the occurrence of some large solar flares. The exact physical mechanism that causes sunquakes is still a topic of discussion, but it is thought to be related to the release of magnetic energy during a flare. This study investigates the temporal and spatial evolution of permanent changes in the magnetic field geometry associated with sunquakes. We analyze a sample of seven acoustically active flaring events that occurred during solar cycle 24. The data used for this analysis were higher cadence (135 s) vector magnetograms acquired with the SDO/HMI instrument. We find that the highly energetic flaring events under investigation may inject enough energy into the photosphere and sub-photosphere to generate acoustic responses observed as sunquakes. By analyzing the changes in magnetic field geometry and strength associated with these events, we aim to shed light on the physical mechanisms that lead to the generation of sunquakes. This work represents an important step towards a better understanding of sunquakes and their underlying physical mechanisms. It also contributes to the development of more accurate models and simulations of these phenomena. Ultimately, this could lead to a better understanding of the physics of solar flares.