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Interplanetary coronal mass ejections (ICMEs) have low proton beta across abroad range of heliocentric distances and a magnetic flux rope structure atlarge scales, making them a unique environment for studying solar windfluctuations. Power spectra of magnetic field fluctuations in 28 ICMEs observedbetween 0.25 and 0.95 au by Solar Orbiter and Parker Solar Probe have beenexamined. At large scales, the spectra were dominated by power contained in theflux ropes. Subtraction of the background flux rope fields reduced the meanspectral index from $-5/3$ to $-3/2$ at $kd_i \leq 10^{-3}$. Rope subtractionalso revealed shorter correlation lengths in the magnetic field. The spectralindex was typically near $-5/3$ in the inertial range at all radial distancesregardless of rope subtraction, and steepened to values consistently below $-3$with transition to kinetic scales. The high-frequency break point terminatingthe inertial range evolved approximately linearly with radial distance and wascloser in scale to the proton inertial length than the proton gyroscale, asexpected for plasma at low proton beta. Magnetic compressibility at inertialscales did not show any significant correlation with radial distance, incontrast to the solar wind generally. In ICMEs, the distinctive spectralproperties at injection scales appear mostly determined by the global flux ropestructure while transition-kinetic properties are more influenced by the lowproton beta; the intervening inertial range appears independent of both ICMEfeatures, indicative of a system-independent scaling of the turbulence.

Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure