A High-resolution Study of Magnetic Field Evolution and Spicular Activity around the Boundary of a Coronal Hole

In this study, we analyze high-spatial-resolution (0.'' 24) magnetograms and high-spatial-resolution (0.'' 10) H alpha off-band (+/- 0.8 angstrom) images taken by the 1.6 m Goode Solar Telescope to investigate the magnetic properties associated with small-scale ejections in a coronal hole boundary region from a statistical perspective. With one and a half hours of optical observations under excellent seeing, we focus on the magnetic structure and evolution by tracking the magnetic features with the Southwest Automatic Magnetic Identification Suite (SWAMIS). The magnetic field at the studied coronal hole boundary is dominated by negative polarity with flux cancellations at the edges of the negative unipolar cluster. In a total of 1250 SWAMIS-detected magnetic cancellation events, similar to 39% are located inside the coronal hole with an average flux cancellation rate of 2.0 x 10(18) Mx Mm(-2) hr(-1), and similar to 49% are located outside the coronal hole with an average flux cancellation rate of 8.8 x 10(17) Mx Mm(-2) hr(-1). We estimated that the magnetic energy released due to flux cancellation inside the coronal hole is six times more than that outside the coronal hole. Flux cancellation accounts for similar to 9.5% of the total disappearance of magnetic flux. Other forms of its disappearance are mainly due to fragmentation of unipolar clusters or merging with elements of the same polarity. We also observed a number of significant small-scale ejections associated with magnetic cancellations at the coronal hole boundary that have corresponding EUV brightenings.