  We use the exact solutions for magnetoacoustic waves in a two dimensional
isothermal atmosphere with uniform inclined magnetic field to calculate the
wave reflection, transmission, and conversion of slow and fast waves incident
from above ($z=\infty$). This is relevant to the question of whether waves
excited by flares in the solar atmosphere can penetrate the Alfv\'en/acoustic
equipartition layer (which we identify as the canopy) to reach the photosphere
with sufficient energy to create sunquakes. It is found that slow waves above
the acoustic cutoff frequency efficiently penetrate (transmit) as acoustic
(fast) waves if directed at a small attack angle to the magnetic field, with
the rest converting to magnetic (slow) waves, in accord with Generalized Ray
Theory. This may help explain the compact nature of seismic sources of
sunquakes identified using seismic holography. The incident slow waves can also
efficiently transmit at low frequency in inclined field due to the reduction in
acoustic cutoff frequency (ramp effect). Incident fast (magnetic) "waves" from
infinity with specified nonzero horizontal wavenumber are necessarily
evanescent, but can carry energy to the equipartition level by tunnelling. It
is found that this can then efficiently convert to acoustic (fast) energy that
can again reach the photosphere as a travelling wave. Overall, there appear to
be ample avenues for substantial compressive wave energy to penetrate the
canopy and impact the photosphere.
