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The dynamics of coronal mass ejections (CMEs) in interplanetary space (IPS) are primarily determined by the interaction of the CME with the interplanetary magnetic field (IMF) and the surrounding solar wind (SW). CMEs are complex magnetized plasma structures in which the magnetic field spirals around a central axis, forming what is known as a flux rope (FR). This FR axis can be oriented at any angle with respect to the ecliptic. Throughout its journey, a CME will encounter IMF and SW in IPS which is neither homogeneous nor isotropic. Consequently, CMEs with different orientations will encounter different ambient medium conditions. It is thus expected that the interaction of the CME with its surrounding environment will vary depending on the orientation of its FR axis, among other factors. This study aims to fill the gap in the understanding of the effect of inclination on CME propagation in the heliosphere. This is achieved by performing simulations with the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) 3D magnetohydrodynamic (MHD) model. This study focuses on two CMEs with nearly identical properties, differing only by their inclination, which are simulated using the spheromak CME implementation in the model. We show the effects of CME orientation on sheath evolution, MHD drag, and non-radial flows in radial, longitudinal, and latitudinal directions, by analyzing the model data from a swarm of 81 virtual spacecrafts scattered across the inner heliospheric domain of EUHFORIA. These results provide new insights into CME dynamics, the understanding of which is critical for improving space weather forecasting.
Martinić et al. (Fri,) studied this question.