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We present a magnetic flux rope (FR) extraction tool for solar coronalmagnetic field modelling data, which builds upon the methodology from Wagner etal. (2023). We apply the scheme to magnetic field simulations of active regionsAR12473 and AR11176. We compare the method to its predecessor and study the 3Dmovement of the newly extracted FRs up to heights of 200 and 300 Mm,respectively. The extraction method is based on the twist parameter and avariety of mathematical morphology algorithms, including the opening transformand the morphological gradient. We highlight the differences between themethods by investigating the circularity of the FRs in the plane we extractfrom. The simulations for the active regions are carried out with atime-dependent data-driven magnetofrictional model (TMFM; Pomoell et al.(2019)). We investigate the FR trajectories by tracking their apex throughoutthe full simulation time span. We demonstrate that this upgraded methodologyprovides the user with more tools and less a-priori assumptions about the FRshape that, in turn, leads to a more accurate set of field lines. Thepropagation analysis yields that the erupting FR from AR12473 showcasesstronger dynamics than the AR11176 FR and a significant deflection during itsascent through the domain. The AR11176 FR appears more stable, though therestill is a notable deflection. This confirms that at these low coronal heights,FRs do undergo significant changes in the direction of their propagation evenfor less dynamic cases. The modelling results are also verified withobservations, with AR12473 being indeed dynamic and eruptive, while AR11176only features an eruption outside of our simulation time window.

The Automatic Identification and Tracking of Coronal Flux Ropes -- Part  II: New Mathematical Morphology-based Flux Rope Extraction Method and  Deflection Analysis