Abstract The solar coronal magnetic field is a pivotal element in the study of eruptive phe-
nomena, and understanding its dynamic evolution has long been a focal point in solar physics.
Numerical models, driven directly by observation data, serve as indispensable tools in investi-
gating the dynamics of the coronal magnetic field. This paper presents a new approach to elec-
tric field inversion, which involves modifying the electric field derived from the DAVE4VM
velocity field using ideal Ohm’s law. The time series of the modified electric field is used as
a boundary condition to drive a full MHD data-driven model, which is applied to simulate
the magnetic field evolution of active region 12673. The simulation results demonstrate that
our method enhances the magnetic energy injection through the bottom boundary, as com-
pared with energy injection calculated directly from the DAVE4VM code, and reproduce of
the evolution of the photospheric magnetic flux. The coronal magnetic field structure is also
in morphological similarity to the coronal loops. This new approach will be applied to the
high-accuracy simulation of eruption phenomena and provide more details on the dynamical
evolution of the coronal magnetic field.