  Coronal magnetic fields evolve quasi statically over long time scales and
dynamically over short time scales. As of now there exists no regular
measurements of coronal magnetic fields, and therefore generating the coronal
magnetic field evolution using the observations of the magnetic field at the
photosphere is of fundamental requirement to understand the origin of the
transient phenomena from the solar active regions. Using the magnetofriction
(MF) approach, we aim to simulate the coronal field evolution in the solar
active region 11429. The MF method is implemented in open source \PC along with
a driver module to drive the initial field with different boundary conditions
prescribed from observed vector magnetic fields at the photosphere. In order to
work with vector potential and the observations, we prescribe three types of
bottom boundary drivers with varying free-magnetic energy. The MF simulation
reproduces the magnetic structure, which better matches to the sigmoidal
morphology exhibited by AIA images at the pre-eruptive time. We found that the
already sheared field further driven by the sheared magnetic field, will
maintain and further build the highly sheared coronal magnetic configuration,
as seen in AR 11429. Data-driven MF simulation is a viable tool to generate the
coronal magnetic field evolution, capturing the formation of the twisted flux
rope and its eruption.

Solar and Stellar Astrophysics