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Magnetic reconnection is essential to release the flux rope during itsejection. The question remains: how does the magnetic reconnection change theflux rope structure? Following the original study of \citet{Qiu2007}, wecompare properties of ICME/MC flux ropes measured at 1 AU and properties ofassociated solar progenitors including flares, filaments, and CMEs. Inparticular, the magnetic field-line twist distribution within interplanetarymagnetic flux ropes is systematically derived and examined. Our analysis showsthat for most of these events, the amount of twisted flux per AU in MCs iscomparable with the total reconnection flux on the Sun, and the sign of the MChelicity is consistent with the sign of helicity of the solar source regionjudged from the geometry of post-flare loops. Remarkably, we find that aboutone half of the 18 magnetic flux ropes, most of them being associated witherupting filaments, have a nearly uniform and relatively low twist distributionfrom the axis to the edge, and the majority of the other flux ropes exhibitvery high twist near the axis, of up to $\gtrsim 5$ turns per AU, whichdecreases toward the edge. The flux ropes are therefore not linear force free.We also conduct detailed case studies showing the contrast of two events withdistinct twist distribution in MCs as well as different flare and dimmingcharacteristics in solar source regions, and discuss how reconnection geometryreflected in flare morphology may be related to the structure of the flux ropeformed on the Sun.

Structures of Interplanetary Magnetic Flux Ropes and Comparison with Their Solar Sources