  Sunspot light bridges are known to exhibit a variety of dynamic and
persistent phenomena such as surges, small-scale jets etc. in the chromosphere
and transition region. While it has generally been proposed that magnetic
reconnection is responsible for this small-scale dynamism, persistent flaring
activity lasting several hours from the same spatial location on a sunspot
light bridge, has rarely been reported. We combine observations from the
Atmospheric Imaging Assembly and the Helioseismic Magnetic Imager on board the
Solar Dynamics Observatory to investigate homologous flaring activity over a
small sunspot light bridge in an emerging flux region. The homologous flares
all produced broad, collimated jets, including a B6.4 class flare. The jets
rise at a speed of about 200 km/s, reach projected heights of about 98 Mm, and
emerge from the same spatial location for nearly 14 hrs, after which they cease
completely. A non-linear force free extrapolation of the photospheric magnetic
field shows a low-lying flux rope connecting the light bridge to a remote
opposite-polarity network. The persistent flares occur as a result of the rapid
horizontal motion of the leading sunspot that causes the relatively vertical
magnetic fields in the adjacent umbra to reconnect with the low-lying flux rope
in the light bridge. Our results indicate that the flaring ceases once the flux
rope has lost sufficient twist through repeated reconnections.
