  The transport of the energy contained in electrons, both thermal and
suprathermal, in solar flares plays a key role in our understanding of many
aspects of the flare phenomenon, from the spatial distribution of hard X-ray
emission to global energetics. Motivated by recent {\em RHESSI} observations
that point to the existence of a mechanism that confines electrons to the
coronal parts of flare loops more effectively than Coulomb collisions, we here
consider the impact of pitch-angle scattering off turbulent magnetic
fluctuations on the parallel transport of electrons in flaring coronal loops.
It is shown that the presence of such a scattering mechanism in addition to
Coulomb collisional scattering can significantly reduce the parallel thermal
and electrical conductivities relative to their collisional values. We provide
illustrative expressions for the resulting thermoelectric coefficients that
relate the thermal flux and electrical current density to the temperature
gradient and the applied electric field. We then evaluate the effect of these
modified transport coefficients on the flare coronal temperature that can be
attained, on the post-impulsive-phase cooling of heated coronal plasma, and on
the importance of the beam-neutralizing return current on both ambient heating
and the energy loss rate of accelerated electrons. We also discuss the possible
ways in which anomalous transport processes have an impact on the required
overall energy associated with accelerated electrons in solar flares.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena;Plasma Physics