  Data-driven time-dependent magnetofrictional modelling (TMFM) of active
region magnetic fields has been proven to be a useful tool to study the corona.
The input to the model is the photospheric electric field that is inverted from
a time series of the photospheric magnetic field. Constraining the complete
electric field, that is, including the non-inductive component, is critical for
capturing the eruption dynamics. We present a detailed study of the effects of
optimisation of the non-inductive electric field on the TMFM of AR12473. We aim
to study the effects of varying the non-inductive electric field on the
data-driven coronal simulations, for two alternative parametrisations. By
varying parameters controlling the strength of the non-inductive electric
field, we wish to explore the changes in flux rope formation and their early
evolution and other parameters, for instance, axial flux and magnetic field
magnitude.The non-inductive electric field component in the photosphere is
critical for energising and introducing twist to the coronal magnetic field,
thereby allowing unstable configurations to be formed. We estimated this
component using an approach based on optimising the injection of magnetic
energy. However, the flux rope formation, evolution and eruption time varies
depending on the values of the optimisation parameters. The flux rope is formed
and has overall similar evolution and properties with a large range of
non-inductive electric fields needed to determine the non-inductive electric
field component that is critical for energising and introducing twist to the
coronal magnetic field. This study shows that irrespective of non-inductive
electric field values, flux ropes are formed and erupted, which indicates that
data-driven TMFM can be used to estimate flux rope properties early in their
evolution without employing a lengthy optimisation process.
