Probing Coronal Mass Ejection Inclination Effects with EUHFORIA

Coronal mass ejections (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). The central FR axis can be oriented at any angle with respect to the ecliptic. Throughout its journey, a CME will encounter int...

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Bibliographic Details
Published in:The Astrophysical journal 2024-10, Vol.974 (2), p.203
Main Authors: Martinić, Karmen, Asvestari, Eleanna, Dumbović, Mateja, Rindlisbacher, Tobias, Temmer, Manuela, Vršnak, Bojan
Format: Article
Language:English
Subjects:
Coronal mass ejection
Drag
Ecliptic
Heliosphere
Inclination
Interplanetary magnetic field
Magnetic fields
Magnetic flux
Magnetic properties
Magnetohydrodynamical simulations
Orientation effects
Parameters
Sheaths
Solar coronal mass ejections
Solar magnetic field
Solar physics
Solar wind
Spacecraft
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Summary:Coronal mass ejections (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). The central FR axis can be oriented at any angle with respect to the ecliptic. Throughout its journey, a CME will encounter interplanetary magnetic fields and solar winds that are neither homogeneous nor isotropic. Consequently, CMEs with different orientations will encounter different ambient medium conditions and, thus, the interaction of a CME with its surrounding environment will vary depending on the orientation of its FR axis, among other factors. This study aims to understand the effect of inclination on CME propagation. We performed simulations with the EUHFORIA 3D magnetohydrodynamic model. This study focuses on two CMEs modeled as spheromaks with nearly identical properties, differing only by their inclination. We show the effects of CME orientation on sheath evolution, MHD drag, and nonradial flows by analyzing the model data from a swarm of 81 virtual spacecraft scattered across the inner heliospheric. We have found that the sheath duration increases with radial distance from the Sun and that the rate of increase is greater on the flanks of the CME. Nonradial flows within the studied sheath region appear larger outside the ecliptic plane, indicating a “sliding” of the interplanetary magnetic field in the out-of-ecliptic plane. We found that the calculated drag parameter does not remain constant with radial distance and that the inclination dependence of the drag parameter cannot be resolved with our numerical setup.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ad7392