  Context: Late on 2013 August 19, a coronal mass ejection (CME) erupted from
an active region located near the far-side central meridian from Earth's
perspective. The event and its accompanying shock were remotely observed by the
STEREO-A, STEREO-B and SOHO spacecraft. The interplanetary counterpart (ICME)
was intercepted by MESSENGER near 0.3 au, and by both STEREO-A and STEREO-B,
near 1 au, which were separated by 78{\deg} in heliolongitude. The main
objective of this study is to follow the radial and longitudinal evolution of
the ICME throughout the inner heliosphere, and to examine possible scenarios
for the different magnetic flux-rope configuration observed on the solar disk,
and measured in situ at the locations of MESSENGER and STEREO-A, separated by
15{\deg} in heliolongitude, and at STEREO-B, which detected the ICME flank.
Results: We find that the magnetic flux-rope structure detected at STEREO-B
belongs to the same ICME detected at MESSENGER and STEREO-A. The opposite
helicity deduced at STEREO-B, might be due to the spacecraft intercepting one
of the legs of the structure far from the flux-rope axis, while STEREO-A and
MESSENGER are crossing through the core of the magnetic flux rope. The
different flux-rope orientations measured at MESSENGER and STEREO-A arise
probably because the two spacecraft measure a curved, highly distorted and
rather complex magnetic flux-rope topology. The ICME may have suffered
additional distortion in its evolution in the inner heliosphere, such as the
west flank is propagating faster than the east flank when arriving 1 au.
Conclusions: This work illustrates how the ambient conditions can significantly
affect the expansion and propagation of the CME/ICME, introducing additional
irregularities to the already asymmetric eruption, and how these complex
structures cannot be directly reconstructed with the current models available.
