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The evolution of the magnetic field and plasma quantities inside a coronalmass ejection (CME) with distance are known from statistical studies using datafrom 1 au monitors, planetary missions, Helios, and Ulysses. This does notcover the innermost heliosphere, below 0.29 au, where no data are yet publiclyavailable. Here, we describe the evolution of the properties of simulated CMEsin the inner heliosphere using two different initiation mechanisms. We comparethe radial evolution of these properties with that found from statisticalstudies based on observations in the inner heliosphere by Helios and MESSENGER.We find that the evolution of the radial size and magnetic field strength isnearly indistinguishable for twisted flux rope from that of writhed CMEs. Theevolution of these properties is also consistent with past studies, primarilywith recent statistical studies using in situ measurements and with studiesusing remote observations of CMEs.

Evolution of CME Properties in the Inner Heliosphere: Prediction for Solar Orbiter and Parker Solar Probe