Evolution of Coronal Mass Ejections in Different Data-driven Solar Wind Conditions

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Abstract
Numerical models of the solar wind and coronal mass ejections (CMEs) utilize photospheric magnetic field observations to prescribe the inner boundary conditions for the plasma solutions. These magnetic field data are available to the community through various observational instruments, prepared via different methodologies and/or flux transport models. The solar wind solution driven by these maps provides the ambient plasma environment into which CMEs travel. Interaction with the surrounding solar wind impacts CME evolution and propagation in the solar corona and inner heliosphere. In this work, we use different input magnetic field maps for the same time period to drive the global Alfvén Wave Solar atmosphere Model. We obtain the ambient solar wind conditions and compare the plasma properties and magnetic morphology in the corona domain to study the influence of the input maps. To understand how the resulting coronal solutions impact CMEs, we launch eruptions described by analytical flux ropes into these data-driven solutions and compare their evolution in the coronal domain (up to 24 R ⊙ radially). The CMEs achieve varying speeds, deceleration rates, propagation directions, mass, and energies while coupling with the background solar wind. We quantify these differences to show that the different input driving maps can significantly impact the simulated CME propagation in the solar wind plasma. This also highlights the importance of understanding the uncertainties associated with data-driven modeling that become increasingly important in operational models and space weather prediction.
Funding Information
  • NASA ∣ SMD ∣ Heliophysics Division (80NSSC24K1104)
  • NASA ∣ SMD ∣ Heliophysics Division (80NSSC22K0892)
  • NSF ∣ Directorate for Geosciences (PHY-202755)
  • NSF ∣ Directorate for Geosciences (2323303)
  • NASA ∣ SMD ∣ Heliophysics Division (80NSSC23K0450)

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