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The relationship between solar eruption and sunspot rotation has been widelyreported, and the underlying mechanism requires to be studied. Here weperformed a full 3D MHD simulation of data-constrained approach to study themechanism of flare eruptions in active region (AR) NOAA 10930, which ischaracterized by continuous sunspot rotation and homologous eruptions. Wereconstructed the potential magnetic field from the magnetogram of Hinode/SOTas the initial condition and drove the MHD system by applying continuoussunspot rotation at the bottom boundary. The key magnetic structure before themajor eruptions and the pre-formed current sheet were derived, which isresponsible for the complex MHD evolution with multiple stages. The majoreruptions were triggered directly by fast reconnection in the pre-formedcurrent sheet above the main polarity inversion line between the two majormagnetic polarities of the AR. Furthermore, our simulation shows the homologouseruption successfully. It has reasonable consistence with observations inrelative strength, energy release, X-ray and H{\alpha} features and timeinterval of eruptions. In addition, the rotation angle of the sunspot beforethe first eruption in the simulation is also close to the observed value. Oursimulation offers a scenario different from many previous studies based onideal instabilities of twisted magnetic flux rope, and shows the importance ofsunspot rotation and magnetic reconnection in efficiently producing homologouseruptions by continuous energy injection and impulsive energy release in arecurrent way.

MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation