Resolve the persistent underestimation of heliospheric magnetic field magnitudes in global MHD models

Determine the physical and/or numerical causes of the systematically low magnetic field amplitudes predicted by global heliospheric magnetohydrodynamic models (e.g., MAS with Wave-Turbulence-Driven heating) relative to in-situ observations at 1 AU, and develop validated model improvements that eliminate this discrepancy.

Background

In the direct comparison for CR2063, the authors note that while many plasma parameters are reasonably captured, the modeled magnetic field strengths remain too low compared to observations.

They emphasize that this is not an isolated issue of the present setup but a broader modeling shortfall reported previously in global heliospheric simulations, citing prior studies that documented the problem. The statement flags the issue as unresolved despite earlier investigations, underscoring a need to identify root causes and corrective strategies.