Speaker
Description
The origin and formation of the solar wind remain an open question in solar physics. One proposed scenario is that some solar wind may arise from coronal hole boundaries via magnetic reconnection, the process that also dominates the evolution of coronal hole boundaries. In this study, we investigate the magnetic field and plasma properties at different parts of the boundary of a large equatorial coronal hole. Differential Emission Measure analysis is used to derive plasma properties at these regions. We also implement the correlation dimension mapping analysis to measure the irregularities of the coronal hole boundary. We find that the leading boundary has a higher temperature, a stronger, more unipolar magnetic field, and a smoother boundary line than the trailing boundary. These differences are hypothesised to be direct consequences of the local magnetic field configurations at the coronal hole boundary: the leading boundary corresponds to large, well-organised coronal loops, and the trailing boundary corresponds to more dispersed, randomly oriented, and smaller magnetic bipoles. These differences in the magnetic field structure may also influence the nature of interchange reconnection at coronal hole boundaries.
