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Dynamical jets are generally found on Light bridges (LBs), which are key tostudying sunspots decays. So far, their formation mechanism is not fullyunderstood. In this paper, we used state-of-the-art observations from the GoodeSolar Telescope, the Interface Region Imaging Spectrograph, theSpectro-Polarimeter on board Hinode and the Atmospheric Imaging Assembly (AIA)on board the Solar Dynamics Observatory to analyze the fan shape jets on LBs indetail. Continuous upward motion of the jets in ascending phase is found fromthe H$\alpha$ velocity, which lasts for 12 minutes and is associated with theH$\alpha$ line wing enhancements. Two mini jets appear upon the bright frontsof the fan shape jets visible in the AIA 171 {\AA} and 193 {\AA} channels, witha time interval as short as 1 minute. Two kinds of small scale convectivemotions are identified in the photospheric images, along with the H$\alpha$line wing enhancements. One seems to be associated with the formation of a newconvection cell and the other manifests as the motion of a dark lane passingthrough the convection cell. The finding of three lobes Stokes V profiles andtheir inversion with NICOLE code indicates that there is magnetic field lineswith opposite polarities in LBs. From the H$\alpha$ -0.8 {\AA} images, we foundribbon like brightenings propagating along the LBs, possibly indicatingslipping reconnection. Our observation supports that the fan shape jets understudy are caused by the magnetic reconnection and photospheric convectivemotions play an important role in triggering the magnetic reconnection.

Signatures of magnetic reconnection at the footpoints of fan shape jets on a light bridge driven by photospheric convective motions