  Extreme ultraviolet (EUV) images from the Atmospheric Imaging Assembly (AIA)
on board the Solar Dynamic Observatory (SDO) are providing new insights into
the early phase of CME evolution. Observations now show the ejection of
magnetic flux ropes from the solar corona and how they evolve into CMEs. These
observations are difficult to interpret in terms of basic physical mechanisms
and quantities. To fully understand CMEs we need to compare equivalent
quantities derived from both observations and theoretical models. To this end
we aim to produce synthesised AIA observations from simluations of a flux rope
ejection. To carry this out we include the role of thermal conduction and
radiative losses, both of which are important for determining the temperature
distribution of the solar corona during a CME. We perform a simulation where a
flux rope is ejected from the solar corona. From the density and temperature of
the plasma in the simulation we synthesise AIA observations. The emission is
then integrated along the line of sight using the instrumental response
function of AIA. We sythesise observations of AIA in the channels at 304 A, 171
A, 335 A, and 94 A. The synthesised observations show a number of features
similar to actual observations and in particular reproduce the general
development of CMEs in the low corona as observed by AIA. In particular we
reproduce an erupting and expanding arcade in the 304 A and 171 A channels with
a high density core. The ejection of a flux rope reproduces many of the
features found in the AIA observations. This work is therefore a step forward
in bridging the gap between observations and models, and can lead to more
direct interpretations of EUV observations in terms of flux rope ejections. We
plan to improve the model in future studies in order to perform a more
quantitative comparison.
