  Alfv\'enic waves have been proposed as an important energy transport
mechanism in coronal loops, capable of delivering energy to both the corona and
chromosphere and giving rise to many observed features, of flaring and
quiescent regions. In previous work, we established that resistive dissipation
of waves (ambipolar diffusion) can drive strong chromospheric heating and
evaporation, capable of producing flaring signatures. However, that model was
based on a simplified assumption that the waves propagate instantly to the
chromosphere, an assumption which the current work removes. Via a ray tracing
method, we have implemented traveling waves in a field-aligned hydrodynamic
simulation that dissipate locally as they propagate along the field line. We
compare this method to and validate against the magnetohydrodynamics code
Lare3D. We then examine the importance of travel times to the dynamics of the
loop evolution, finding that (1) the ionization level of the plasma plays a
critical role in determining the location and rate at which waves dissipate;
(2) long duration waves effectively bore a hole into the chromosphere, allowing
subsequent waves to penetrate deeper than previously expected, unlike an
electron beam whose energy deposition rises in height as evaporation reduces
the mean-free paths of the electrons; (3) the dissipation of these waves drives
a pressure front that propagates to deeper depths, unlike energy deposition by
an electron beam.
