Orateur
Description
Magnetic reconnection at Earth’s magnetopause is the key process controlling the coupling between the solar wind and the magnetosphere, enabling plasma and magnetic flux from the interplanetary medium to enter an otherwise largely closed cavity. A central question is where reconnection develops along the magnetopause, since its location strongly influences the efficiency of this coupling. Despite decades of work, predicting the reconnection line remains difficult because the process is inherently multiscale, while spacecraft observations provide only local, in situ measurements and kinetic numerical modeling at large scale is extremely costly.
Recent progress has become possible by combining decades of observations from multiple missions with innovative machine-learning-based analysis. These approaches have yielded new insight into the environmental and physical constraints that govern both the location of the dayside reconnection line and the reconnection efficiency. This presentation will review these advances, from large-scale statistical results based on in situ measurements to new models of the X-line and recent developments in multiscale modeling to offer a complementary perspective on magnetopause reconnection.