  Magnetic reconnection is essential to release the flux rope during its
ejection. The question remains: how does the magnetic reconnection change the
flux rope structure? Following the original study of \citet{Qiu2007}, we
compare properties of ICME/MC flux ropes measured at 1 AU and properties of
associated solar progenitors including flares, filaments, and CMEs. In
particular, the magnetic field-line twist distribution within interplanetary
magnetic flux ropes is systematically derived and examined. Our analysis shows
that for most of these events, the amount of twisted flux per AU in MCs is
comparable with the total reconnection flux on the Sun, and the sign of the MC
helicity is consistent with the sign of helicity of the solar source region
judged from the geometry of post-flare loops. Remarkably, we find that about
one half of the 18 magnetic flux ropes, most of them being associated with
erupting filaments, have a nearly uniform and relatively low twist distribution
from the axis to the edge, and the majority of the other flux ropes exhibit
very high twist near the axis, of up to $\gtrsim 5$ turns per AU, which
decreases toward the edge. The flux ropes are therefore not linear force free.
We also conduct detailed case studies showing the contrast of two events with
distinct twist distribution in MCs as well as different flare and dimming
characteristics in solar source regions, and discuss how reconnection geometry
reflected in flare morphology may be related to the structure of the flux rope
formed on the Sun.
