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Solar flares and coronal mass ejections (CMEs) are the most powerfulexplosions in the Sun. They are major sources of potentially destructive spaceweather conditions. However, the possible causes of their initiation remaincontroversial. By using high resolution data observed by NST of BBSO,supplemented by Solar Dynamics Observatory (SDO) observations, we presentunusual observations of a small-scale emerging flux rope near a large sunspot,whose eruption produced an M-class flare and a coronal mass ejection. Thepresence of the small-scale flux rope was indicated by static nonlinear forcefree field (NLFFF) extrapolation as well as data-driven MHD modeling of thedynamic evolution of the coronal 3D magnetic field. During the emergence of theflux rope, rotation of satellite sunspots at the footpoints of the flux ropewas observed. Meanwhile, the Lorentz force, magnetic energy, vertical current,and transverse fields were increasing during this phase. The free energy fromthe magnetic flux emergence and twisting magnetic fields is sufficient to powerthe M-class flare. These observations for the first time present the completeprocess from the emergence of the small-scale flux rope to the production ofsolar eruptions.

The eruption of a small-scale emerging flux rope as the driver of an M-class flare and a coronal mass ejection