Relationship of ICME Composition Signatures with Solar Activity during 2009-2025
Coronal Mass Ejections (CMEs) are among the most energetic solar eruptions, expelling magnetized plasma from the corona into interplanetary space. Their interplanetary counterparts, known as Interplanetary Coronal Mass Ejections (ICMEs), retain distinct compositional signatures that reflect the physical conditions of their solar source regions. This study presents a statistical analysis of ICME composition dependence on solar activity during 2009--2025, covering Solar Cycle (SC) 24 and the ascending phase of SC~25 through its maximum, and compares the results with SC~23 studied by \citet{Song+etal+2021}. Using data from the Solar Wind Ion Composition Spectrometer (SWICS) aboard the Advanced Composition Explorer (ACE), we examined the average iron charge state ($\langle Q_{\rm Fe}\rangle$), ionic ratios (C$^{6+}$/C$^{5+}$ and O$^{7+}$/O$^{6+}$), and the elemental abundance ratio (Fe/O) for 307 ICMEs listed in the Richardson and Cane ICME catalog. The results show strong positive correlations of $\langle Q_{\rm Fe}\rangle$ ($r$~=~0.86) and O$^{7+}$/O$^{6+}$ ($r$~=~0.85) with the annual sunspot number (SSN), whereas C$^{6+}$/C$^{5+}$ exhibits a weak correlation ($r$~=~0.17) primarily due to SWICS~2.0 upper-end saturation truncation that suppresses the solar maximum signal, and Fe/O a moderate correlation ($r$~=~0.57). The Fe/O ratio, a proxy for the First Ionization Potential (FIP) effect, displayed elevated values during the maxima of both SC~24 and SC~25, suggesting enhanced elemental fractionation during periods of increased magnetic activity. Comparing with SC~23, we find that the overall solar cycle dependence of ICME composition persists across cycles, though with notable quantitative differences attributed to the different magnetic activity levels between cycles. These findings confirm that ICME compositional signatures are strongly modulated by the solar cycle.