The interaction of open and closed field lines at coronal holeboundaries is widely accepted to be due to interchange magneticreconnection. To date, it is unclear how the boundaries vary on shorttimescales and at what velocity this occurs. Here, we describe anautomated boundary tracking method used to determine coronal holeboundary displacements on short timescales. The boundary displacementswere found to be isotropic and to have typical expansion/contractionspeeds of ≤2 km s-1, which indicate magnetic reconnectionrates of ≤3 x 10. The observed displacements were usedin conjunction with the interchange reconnection model to derivetypical diffusion coefficients of ≤3 x 1013cm2 s-1.These results are consistent with an interchange reconnection processin the low corona driven by the random granular motions of open andclosed fields in the photosphere.
Authors: Larisza D. Krista, Peter T. Gallagher, D. Shaun Bloomfield
Publication Status: ApJL (Accepted)
Last Modified: 2011-03-15 14:49