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Using high-resolution images from 1.6 m New Solar Telescope (NST) at Big BearSolar Observatory (BBSO), we report the direct evidence of chromosphericreconnection at the polarity inversion line (PIL) between two small oppositepolarity sunspots. Small jet-like structures (with velocities of ~20-55 km/s)were observed at the reconnection site before the onset of the first M1.0flare. The slow rise of untwisting jets was followed by the onset of coolplasma inflow (~10 km/s) at the reconnection site, causing the onset of atwo-ribbon flare. The reconnection between two sheared J-shaped cool H$\alpha$loops causes the formation of a small twisted flux rope (S shaped) in thechromosphere. In addition, Helioseismic and Magnetic Imager (HMI) magnetogramsshow the flux cancellation (both positive and negative) during the first M1.0flare. The emergence of negative flux and cancellation of positive flux (withshear flows) continue until the successful eruption of the flux rope. The newlyformed chromospheric flux rope becomes unstable and rises slowly with the speedof ~108 km/s during a second C8.5 flare that occurred after ~3 hours of thefirst M1.0 flare. The flux rope was destroyed by repeated magnetic reconnectioninduced by its interaction with the ambient field (fan-spine toplology) andlooks like an untwisting surge (~170 km/s) in the coronal images recorded bySolar Dynamic Observatory/Atmospheric Imaging Assembly (SDO/AIA). Theseobservations suggest the formation of a chromospheric flux rope (by magneticreconnection associated with flux cancellation) during the first M1.0 flare andits subsequent eruption/disruption during the second C8.5 flare.

Formation and Eruption of a Small Flux Rope in the Chromosphere Observed by NST, IRIS, and SDO