L-Value and Energy Dependence of 0.1-50 keV O+, He+, and H+ Ions tor CME and CIR Storms Over the Entire Van Allen Probes Era

Plain Language Summary O+, He+, and H+ ions having energies ranging from similar to 10 eV to 50 keV contribute to a majority of the ring current density that provides significant information about the important processes in the inner magnetosphere. In this study, we acquire high-resolution data over the entire Van Allen Probes era to understand storm time dynamics of ion fluxes for the two different categories of solar wind drivers. We find a characteristic difference upon correlating the ion flux enhancement during the storm main phase with the solar wind parameters and strength of the magnetic storm at different L-values and energies for both the category of solar wind drivers. Not all the energies and L-values respond in a similar manner. Moreover, O+, He+, and H+ do not appear at the spacecraft location for the same duration of time. The time duration for which the ion fluxes remain at high is more for Corotating Interaction Region (CIR)-driven storms than Coronal Mass Ejected (CME) ones. Our studies give a comprehensive overview of spatio-temporal characteristics of the inner magnetospheric O+, He+, and H+ ions at different energies using a long-term data set for CME and CIR-driven geomagnetic storms. Our studies report the first observation of L-value and energy sorted correlation of differential fluxes of 0.1-50 keV O+, He+, and H+ ions with different geophysical parameters for 29 Coronal Mass Ejected (CME) and 40 Corotating Interaction Region (CIR)-driven geomagnetic storms during the entire Van Allen Probes era. For both solar wind drivers, ions with >= 1 keV energies show more variability in response to the solar wind changes, while the lower energy (<1 keV) ions are relatively stable. During the in-storm interval, O+ ions show maximum flux enhancement and become further prominent during CME storms. O+ ion (>= 10 keV) fluxes show good correlation with - VswBz, and Sym-H index during CME-driven storms in the L similar to 2.5-5.5. Apart from this, the average duration of persistence ((At)) for enhanced fluxes is higher for CIR-driven storms with ((o)+ >(He+) >(H+) at E <= 50 keV in the L similar to 2.5-5.5. Moreover, the observed value of (t) (where i is O+, H+ or He+) increases with the increasing L. We discuss the plausible mechanisms to provide a comprehensive overview of L-values and energy sorted O+, He+ and H+ ion dynamics for two different categories of solar wind drivers.