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With high-resolution narrowband He I 10830 \r{A} filtergrams from GST, wegive an extensive analysis for 4 granular sized microeruptions which appear asthe gentle ejection of material in He I 10830 \r{A} band. The analysis wasaided with the EUV data from AIA and line-of-sight magnetograms from HMI onboard SDO. The microeruptions are situated on magnetic polarity inversion lines(PILs), and their roots are accurately traced down to intergranular lanes.Their durations are different, two microeruptions are repetitive microjets,lasting ~ 50 and 27 minutes respectively, while the other two events aresingular, lasting ~ 5 minutes. For the two microjets, they are continuous andrecurrent in He I 10830 \r{A} band, and the recurrence is quasi-periodic withthe period of ~ 5 minutes. We found that only transient co-spatial EUVbrightenings are observed for the longer duration microjets and EUVbrightenings are absent for the two singular microeruptions. What is essentialto the longer duration microjets is that granules with the concentration ofpositive magnetic field persistently transport the magnetic field to the PILs,canceling the opposite magnetic flux and making the base of the two microjetsand the underlying granules migrate with the speed of ~ 0.25 and 1.0 km/s. Theobservations support the scenario of magnetic reconnection for thequasi-periodic microjets and further show that the reconnection continuouslygenerates multi-temperature components, especially the cool component withchromospheric temperature. In addition, the ongoing reconnection is modulatedby p-mode oscillations inside the Sun.

Quasi-periodic microjets driven by granular advection as observed with high-resolution imaging at He I 10830 \r{A}