  Burst-like events with signatures in the UV are often observed co-spatial to
strong line-of-sight photospheric magnetic fields. Several authors, for
example, have noted the spatial relationship between Ellerman bombs (EBs) and
Moving Magnetic Features (MMFs), regions of flux which disconnect from a
sunspot or pore before propagating away in the moat flow and often displaying
evidence of cancellation. In this article, data collected by the Solar Dynamics
Observatory's Helioseismic and Magnetic Imager and Atmospheric Imaging Assembly
are analysed in an attempt to understand the potential links between such
cancellation and UV burst formation. Two MMFs from AR 11579, three bi-poles
from AR 11765, and six bi-poles (four of which were co-spatial to IRIS bursts)
in AR 11850 were identified for analysis. All of these cancellation features
were found to have lifetimes of the order hours and cancellation rates of the
order 10^14-10^15 Mx s^-1. H-alpha line wing data from the Dunn Solar
Telescope's Interferometric BIdimensional Spectrometer were also available for
AR 11579 facilitating a discussion of links between MMFs and EBs. Using an
algebraic model of photospheric magnetic reconnection, the measured
cancellation rates are then used to ascertain estimates of certain quantities
(such as up-flow speeds, jet extents, and potential energy releases) which
compared reasonably to the properties of EBs reported within the literature.
Our results suggest that cancellation rates of the order measured here are
capable of supplying enough energy to drive certain UV bursts (including EBs),
however, they are not a guaranteeing condition for burst formation.
