Authors: Yakub Olufadi (University of New Hampshire), Nada AlHadda (University of New Hampshire), Noe Lugaz (University of New Hampshire), Bin Zhuang (University of New Hampshire), Charles Farrugia, (University of New Hampshire).

We investigate how the magnetic and plasma properties of coronal mass ejections (CMEs) evolve with heliocentric distance and solar cycle phase, with the aim of disentangling radial evolution effects from solar-cycle-dependent effects. Using in situ CME observations from multiple spacecraft spanning a broad range of heliocentric distances, we examine magnetic ejecta (ME) and sheath properties during the active phase (AP) and quiet phase (QP) of the solar cycle. We analyze the radial evolution of CME magnetic-field strength, characteristic duration scales, magnetic-field behavior in minimum variance analysis (MVA) coordinates, and plasma properties, including bulk speed (Vp), expansion speed (Vexp), and proton density (Np​), where sufficient event coverage exists in both AP and QP. This framework allows us to distinguish trends primarily associated with CME propagation and expansion from those more directly related to solar-cycle conditions. We further statistically evaluate the significance of the observed differences between AP and QP events throughout their heliocentric evolution.