The physical mechanisms of helium abundance ( ) depletion in the corona and solar wind are closely linked to coronal heating, solar wind origin, and acceleration processes. The relationships between the in the solar wind and the properties and activity of the source regions are crucial for understanding the depletion of . We aim to investigate the impact of active region (AR) activity and properties on the in the solar wind. First, we established the link between carefully selected ARs and the solar wind. Then, the AR chromospheric activity was quantitatively investigated using observations from the Atmospheric Imaging Assembly and Helioseismic Magnetic Imager on board the Solar Dynamics Observatory. The AR temperatures were derived with the differential emission measure method. We also statistically analyzed the in the solar wind with higher and lower charge states during solar cycles 23 and 24. The parameters of solar wind were measured by the instruments on board ACE and Wind. We find that an AR with greater chromospheric activity has higher in its associated solar wind. The statistical analysis shows that the median in solar wind with higher charge states is higher than in solar wind with lower charge states. We conclude that chromospheric activity, primarily chromospheric evaporation processes, is possibly the main heating and transportation mechanism leading to a higher in the corona and solar wind. This could also reasonably explain the variation in in AR solar wind during different solar activity phases and the higher in AR solar wind compared to quiet Sun solar wind.
Ma et al. (Thu,) studied this question.