  Interplanetary Coronal Mass Ejections (ICMEs) originate from the eruption of
complex magnetic structures occurring in our star's atmosphere. Determining the
general properties of ICMEs and the physical processes at the heart of their
interactions with the solar wind is a hard task, in particular using only
unidimensional in situ profiles. Thus, these phenomena are still not well
understood. In this study we simulate the propagation of a set of flux ropes in
order to understand some of the physical processes occurring during the
propagation of an ICME such as their growth or their rotation. We present
simulations of the propagation of a set of flux ropes in a simplified solar
wind. We consider different magnetic field strengths and sizes at the
initiation of the eruption, and characterize their influence on the properties
of the flux ropes during their propagation. We use the 3D MHD module of the
PLUTO code on an Adaptive Mesh Refinement grid. The evolution of the magnetic
field of the flux rope during the propagation matches evolution law deduced
from in situ observations. We also simulate in situ profiles that spacecraft
would have measured at the Earth, and we compare with the results of
statistical studies. We find a good match between simulated in situ profiles
and typical profiles obtained in these studies. During their propagation, flux
ropes interact with the magnetic field of the wind but still show realistic
signatures of ICMEs when analyzed with synthetic satellite crossings. We also
show that flux ropes with different shapes and orientations can lead to similar
unidimensional crossings. This warrants some care when extracting magnetic
topology of ICMEs using unidimensional crossings.
