Mechanisms for the rigid rotation of coronal holes
The rotation of coronal holes is modeled in terms of a current-free coronal magnetic field in which holes are the footpoint locations of open field lines. It is shown that ongoing field-line reconnection allows the holes to rotate quasi-rigidly with their outer-coronal extensions. The results suggest that a strong axisymmetric field component may be responsible for the prolonged rigid rotation of large meridional holes during the declining phase of the sunspot cycle.