Results from a revisit to the K-2V bright points

We have used pairs of temporally simultaneous Call K-line spectroheliograms and magnetic area scans to search for spatial correlation between the CaII K-2V bright points in the interior of the network and corresponding magnet ic elements. We find that about 60% of the K-2V bright points spatially coi ncide with magnetic elements of flux density > 4 Mx cm(-2). About 25% of th e K-2V bright points with equally enhanced emission lie over bipole element s where the fields are > 4 Mx cm(-2) for both polarity elements which merge and presumably cancel and result in low fields. The rest, 15%, of the brig ht points coincide with areas of fields < 4 Mx cm(-2) which is the noise le vel set by us for the magnetic scans. When magnetic elements of opposite po larity merge and form bipoles, the associated K-2V bright points show exces s emission. Although such excess emission is a magnetic-field-drive phenome non, the measured value of the field at the site of the bipole is typically low and these cases would therefore be excluded in the count of coincidenc es of excess emission with excess magnetic fields. In our opinion, these ca ses of excess emission at the sites of the bipoles, as well as at the sites of fields > 4 Mx cm(-2), are both instances of magnetic field-related emis sions. If the former are not taken into account as coincidences, the correl ation will drop down and this might be interpreted as not an obvious correl ation. Our present results, taking into account the low fields of merging b ipoles, establish the association of K-2V bright points with magnetic eleme nts.