The hard X-ray flux ratio R of the footpoint sources to the loop-top source has been used for investigation of a non-thermal electrons propagation in solar flares. Considering the mission-long Yohkoh Hard X-ray Telescope database we found that the ratio R decreases with the height h of a flare loop, which we interpret as an effect of converging field geometry. Two branches seen in the R-h diagram we consider as a proof that in the solar corona exist two kinds of magnetic loops: a more-converged that are more frequent (above 80%) and a less-converged that are less frequent (below 20%). A lack of any correlation between the ratio R and the column depth N along the flare loop can be caused generally by a more complex configuration of investigated events than a single loop.
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