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Coronal magnetic fields evolve quasi statically over long time scales anddynamically over short time scales. As of now there exists no regularmeasurements of coronal magnetic fields, and therefore generating the coronalmagnetic field evolution using the observations of the magnetic field at thephotosphere is of fundamental requirement to understand the origin of thetransient phenomena from the solar active regions. Using the magnetofriction(MF) approach, we aim to simulate the coronal field evolution in the solaractive region 11429. The MF method is implemented in open source \PC along witha driver module to drive the initial field with different boundary conditionsprescribed from observed vector magnetic fields at the photosphere. In order towork with vector potential and the observations, we prescribe three types ofbottom boundary drivers with varying free-magnetic energy. The MF simulationreproduces the magnetic structure, which better matches to the sigmoidalmorphology exhibited by AIA images at the pre-eruptive time. We found that thealready sheared field further driven by the sheared magnetic field, willmaintain and further build the highly sheared coronal magnetic configuration,as seen in AR 11429. Data-driven MF simulation is a viable tool to generate thecoronal magnetic field evolution, capturing the formation of the twisted fluxrope and its eruption.

Data-driven simulations of magnetic field evolution in Active Region 11429: Magneto-friction method using PENCIL code