  We present a magnetic flux rope (FR) extraction tool for solar coronal
magnetic field modelling data, which builds upon the methodology from Wagner et
al. (2023). We apply the scheme to magnetic field simulations of active regions
AR12473 and AR11176. We compare the method to its predecessor and study the 3D
movement of the newly extracted FRs up to heights of 200 and 300 Mm,
respectively. The extraction method is based on the twist parameter and a
variety of mathematical morphology algorithms, including the opening transform
and the morphological gradient. We highlight the differences between the
methods by investigating the circularity of the FRs in the plane we extract
from. The simulations for the active regions are carried out with a
time-dependent data-driven magnetofrictional model (TMFM; Pomoell et al.
(2019)). We investigate the FR trajectories by tracking their apex throughout
the full simulation time span. We demonstrate that this upgraded methodology
provides the user with more tools and less a-priori assumptions about the FR
shape that, in turn, leads to a more accurate set of field lines. The
propagation analysis yields that the erupting FR from AR12473 showcases
stronger dynamics than the AR11176 FR and a significant deflection during its
ascent through the domain. The AR11176 FR appears more stable, though there
still is a notable deflection. This confirms that at these low coronal heights,
FRs do undergo significant changes in the direction of their propagation even
for less dynamic cases. The modelling results are also verified with
observations, with AR12473 being indeed dynamic and eruptive, while AR11176
only features an eruption outside of our simulation time window.
