  Coronal mass ejections (CMEs) represent one type of the major eruption from
the Sun. Their interplanetary counterparts, the interplanetary CMEs (ICMEs),
are the direct manifestations of these structures when they propagate into the
heliosphere and encounter one or more observing spacecraft. The ICMEs generally
exhibit a set of distinctive signatures from the in-situ spacecraft
measurements. A particular subset of ICMEs, the so-called Magnetic Clouds
(MCs), is more uniquely defined and has been studied for decades, based on
in-situ magnetic field and plasma measurements. By utilizing the latest
multiple spacecraft measurements and analysis tools, we report a detailed study
of the internal magnetic field configuration of an MC event observed by both
the Solar Orbiter (SO) and Wind spacecraft in the solar wind near the Sun-Earth
line. Both two-dimensional (2D) and three-dimensional (3D) models are applied
to reveal the flux rope configurations of the MC. Various geometrical as well
as physical parameters are derived and found to be similar within error
estimates for the two methods. These results quantitatively characterize the
coherent MC flux rope structure crossed by the two spacecraft along different
paths. The implication for the radial evolution of this MC event is also
discussed.
