  Solar flares are dramatic events in which magnetic reconnection in the corona
leads to heating of plasma to tens of MK and acceleration of particles to high
energies. They also centrally involve transport between the corona (where the
magnetic reconnection occurs) and the lower solar atmosphere (where most energy
is radiated from). There is substantial evidence for the presence of Alfv\'enic
waves/turbulence in solar flares, for example, in the ubiquitous nonthermal
broadening of flare spectral lines. The physical role that Alfv\'enic waves
have in the flare has attracted considerable attention, especially since
2007-2010. This article reviews what spectroscopic observations reveal about
the properties and importance of Alfv\'enic waves, turbulence and transport in
solar flares; mechanisms for wave excitation by magnetic reconnection at high
Lundquist numbers and braking of the sunward reconnection jet; and models of
wave energy transport to the lower atmosphere and the resulting heating and
dynamics. The article finishes with discussion of the outlook for new progress.
