FRiED: A novel three-dimensional model of coronal mass ejections

Abstract

We present a novel three-dimensional (3D) model of coronal mass ejections (CMEs) that unifies all key evolutionary aspects of CMEs and encapsulates their 3D magnetic field configuration. This fully analytic model is capable of reproducing the global geometrical shape of a CME with all major deformations taken into account, i.e., deflection, rotation, expansion, "pancaking", front flattening and rotational skew. Encapsulation of 3D magnetic structure allows the model to reproduce in-situ measurements of magnetic field for trajectories of spacecraft-CME encounters of any degree of complexity. As such, the model can be used single-handedly for consistent analysis of both remote and in-situ observations of CMEs at any heliocentric distance. We demonstrate the latter by successfully applying the model for analysis of two CMEs.

References in corpus (4)

• Global Trends of CME Deflections Based on CME and Solar Parameters
• Three-dimensional evolution of erupted flux ropes from the Sun (2-20 Rs) to 1 AU
• Quantitative model for the generic 3D shape of ICMEs at 1 AU
• Assessing the Constrained Harmonic Mean Method for Deriving the Kinematics of ICMEs with a Numerical Simulation

Cited by in corpus (13)

• Observation-based modelling of magnetised Coronal Mass Ejections with EUHFORIA
• Determining the Intrinsic CME Flux Rope Type Using Remote-sensing Solar Disk Observations
• Quantifying errors in 3D CME parameters derived from synthetic data using white-light reconstruction techniques
• Implementation and validation of the FRi3D flux rope model in EUHFORIA
• CMEs and SEPs During November-December 2020: A Challenge for Real-Time Space Weather Forecasting
• Modelling a multi-spacecraft coronal mass ejection encounter with EUHFORIA
• The effect of stream interaction regions on ICME structures observed in longitudinal conjunction
• Using the Coronal Evolution to Successfully Forward Model CMEs' In Situ Magnetic Profiles
• Coronal mass ejection deformation at 0.1 au observed by WISPR
• Tracking the 3D evolution of a halo coronal mass ejection using the revised cone model
• Improving the Arrival Time Estimates of Coronal Mass Ejections by Using Magnetohydrodynamic Ensemble Modeling, Heliospheric Imager data, and Machine Learning
• Modelling the interaction of Alfvénic fluctuations with coronal mass ejections in the low solar corona
• Earth-affecting Solar Transients: A Review of Progresses in Solar Cycle 24