Using the "enthalpy-based thermal evolution of loops" (EBTEL) model, weinvestigate the hydrodynamics of the plasma in a flaring coronal loop in whichheat conduction is limited by turbulent scattering of the electrons thattransport the thermal heat flux. The EBTEL equations are solved analytically ineach of the two (conduction-dominated and radiation-dominated) cooling phases.Comparison of the results with typical observed cooling times in solar flaresshows that the turbulent mean free-path $\lambda_T$ lies in a rangecorresponding to a regime in which classical (collision-dominated) conductionplays at most a limited role. We also consider the magnitude and duration ofthe heat input that is necessary to account for the enhanced values oftemperature and density at the beginning of the cooling phase and for theobserved cooling times. We find through numerical modeling that in order toproduce a peak temperature $\simeq 1.5 \times 10^7$~K and a 200~s cooling timeconsistent with observations, the flare heating profile must extend over asignificant period of time; in particular, its lingering role must be takeninto consideration in any description of the cooling phase. Comparison withobservationally-inferred values of post-flare loop temperatures, densities, andcooling times thus leads to useful constraints on both the magnitude andduration of the magnetic energy release in the loop, as well as on the value ofthe turbulent mean free-path $\lambda_T$.
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