Key Influence of Photospheric Magnetic Fields on Solar Wind Heavy-ion Properties

Because heavy-ion abundance ratios and charge states are largely stable within several solar radii of the Sun, they are widely used to diagnose solar wind source regions and the underlying energy-release processes. However, the relationship between these heavy-ion properties and the magnetic field types of their corresponding source regions remains not fully understood. In this work, we construct a data set of 74 events spanning 1998–2017, each providing a complete linkage between the solar source-region magnetic field configuration, coronal mass ejection (CME) properties, and the corresponding in situ interplanetary CME observations. Our analysis demonstrates that the source-region magnetic morphology is a primary parameter governing solar wind heavy-ion charge states, whereas its influence on the heavy-ion abundance ratio is comparatively weaker. For a given magnetic field type, heavy-ion abundances and ionization levels increase exponentially with the strength of associated X-class flares and are further modulated by the longitudinal location of the eruption source region.