  We report and examine the observation of an unusual and rare in-situ electron
observation associated with a solar type III radio burst on 24 December 1996.
This radio event was accompanied by high energy electrons, measured by the
Solid State Telescope (SST) on-board WIND spacecraft. The type III radio
emission started at $\approx$ 13:10~UT and was associated to a C2.1 GOES-class
flare whose maximum was at 13:11 UT and hosted by the active region NOAA
8007/8004, located on the west limb at N05$^\circ$ W74$^\circ$/N06$^\circ$
W85$^\circ$. During this event, the observation of an electron energy
distribution likely to be associated with the radio emission was registered.
The electrons arrive at the spacecraft predominantly from the anti-solar
direction, suggesting that their general motion is Sunward along a closed
magnetic field line. Leblanc et al. (1999) propose a model in which energetic
electrons are injected into a coronal flux tube at one of its footpoints,
releasing standard type-III emission. As the magnetic field then directs them
back toward the magnetic-conjugate footpoint of the first, the electrons
release subsequent emission whose radio profile is a quasi-time reversal of the
standard. We have constructed a cylindrical flux-rope facsimile of this
scenario that reproduces the U-burst profiles. We also report observational
features indicating a secondary electron energy distribution and propose a
scenario that explains this feature.
