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Context. Coronal mass ejections (CMEs) are the main driver of solar winddisturbances near Earth. When directed towards us, the internal magnetic fieldof the CME can interact with the Earth`s magnetic field and cause geomagneticstorms. In order to better predict and avoid damage coming from such events,the optimized heliospheric model Icarus has been implemented. Aims. The impactof a CME at Earth is greatly affected by its internal magnetic field structure.The aim of this work is to enable modelling the evolution of the magnetic fieldconfiguration of the CME throughout its propagation in Icarus. The focus of thestudy is on the global magnetic structure of the CME and its evolution andinteraction with the solar wind. Methods. The magnetized CME model that isimplemented in Icarus is the Linear Force-Free Spheromak and is imported fromEUHFORIA. Advanced techniques, such as grid stretching and AMR are applied.Different AMR levels are applied in order to obtain high resolution locally,where needed. The results of all the simulations are compared in detail and thewall-clock times of the simulations are provided. Results. The results from theperformed simulations are analyzed. The arrival time is better approximated bythe EUHFORIA simulation, with the CME shock arriving 1.6 and 1.09 hours laterthan in the AMR level 4 and 5 simulations, respectively. The profile featuresand variable strengths are best modelled by Icarus simulations with AMR level 4and 5. Conclusions. The arrival time is closer to the observed time in theEUHFORIA simulation, but the profiles of the different variables show morefeatures and details in the Icarus simulations. Considering the smalldifference in the modelled results, and the large difference in computationalresources, the AMR level 4 simulation is considered to have performed the best.

The effect of AMR and grid stretching on the magnetized CME model in Icarus