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Magnetic clouds are a subset of interplanetary coronal mass ejections\udcharacterized by a smooth rotation in the magnetic field direction, which is\udinterpreted as a signature of a magnetic flux rope. Suprathermal electron\udobservations indicate that one or both ends of a magnetic cloud typically\udremain connected to the Sun as it moves out through the heliosphere. With\uddistance from the axis of the flux rope, out toward its edge, the magnetic\udfield winds more tightly about the axis and electrons must traverse longer\udmagnetic field lines to reach the same heliocentric distance. This increased\udtime of flight allows greater pitch-angle scattering to occur, meaning\udsuprathermal electron pitch-angle distributions should be systematically\udbroader at the edges of the flux rope than at the axis. We model this effect\udwith an analytical magnetic flux rope model and a numerical scheme for\udsuprathermal electron pitch-angle scattering and find that the signature of a\udmagnetic flux rope should be observable with the typical pitch-angle\udresolution of suprathermal electron data provided ACE's SWEPAM instrument.\udEvidence of this signature in the observations, however, is weak, possibly\udbecause reconnection of magnetic fields within the flux rope acts to intermix\udflux tubes

The expected imprint of flux rope geometry on suprathermal electrons in magnetic clouds