TRACE Observations of Changes in Coronal Hole Boundaries

Solar coronal holes (CHs) are large regions of the corona magnetically open to interplanetary space. The nearly rigid north -aEuro parts per thousand south CH boundaries (CHBs) of equatorward extensions of polar CHs are maintained while the underlying photospheric fields rotate differentially, so interchange magnetic reconnection is presumed to be occurring continually at the CHBs. The time and size scales of the required reconnection events at CHBs have not been established from previous observations with soft X-ray images. We use TRACE 195 observations on 9 December 2000 of a long-lived equatorial extension of the negative-polarity north polar CH to look for changes of a parts per thousand(3)aEuro parts per thousand 5 arcsec to > 20 arcsec at the western CHB. Brightenings and dimmings are observed on both short (a parts per thousand aEuro parts per thousand 5 minutes) and long (a parts per thousand aEuro parts per thousand 7 hours) time scales, but the CHB maintains its quasi-rigid location. The transient CHB changes do not appear associated with either magnetic field enhancements or the changes in those field enhancements observed in magnetograms from the Michelson Doppler Imager (MDI) on SOHO. In seven hours of TRACE observations we find no examples of the energetic jets similar to those observed to occur in magnetic reconnection in polar plumes. The lack of dramatic changes in the diffuse CHB implies that gradual magnetic reconnection occurs high in the corona with large (a parts per thousand(3)aEuro parts per thousand 10A degrees) loops and/or weak coronal fields. We compare our results with recent observations of active regions at CHBs. We also discuss how the magnetic polarity symmetry surrounding quasi-rigid CHs implies an asymmetry in the interchange reconnection process and a possible asymmetry in the solar wind composition from the eastern and western CHB source regions.