The evolution of the magnetic field and plasma quantities inside a coronal
mass ejection (CME) with distance are known from statistical studies using data
from 1 au monitors, planetary missions, Helios, and Ulysses. This does not
cover the innermost heliosphere, below 0.29 au, where no data are yet publicly
available. Here, we describe the evolution of the properties of simulated CMEs
in the inner heliosphere using two different initiation mechanisms. We compare
the radial evolution of these properties with that found from statistical
studies based on observations in the inner heliosphere by Helios and MESSENGER.
We find that the evolution of the radial size and magnetic field strength is
nearly indistinguishable for twisted flux rope from that of writhed CMEs. The
evolution of these properties is also consistent with past studies, primarily
with recent statistical studies using in situ measurements and with studies
using remote observations of CMEs.