  Magnetic reconnection in the solar corona is thought to be unstable to the
formation of multiple interacting plasmoids, and previous studies have shown
that plasmoid dynamics can trigger MHD waves of different modes propagating
outward from the reconnection site. However, variations in plasma parameters
and magnetic field strength in the vicinity of a coronal reconnection site may
lead to wave reflection and mode conversion. In this paper we investigate the
reflection and refraction of fast magnetoacoustic waves near a reconnection
site. Under a justified assumption of an analytically specified Alfv\'{e}n
speed profile, we derive and solve analytically the full wave equation
governing propagation of fast mode waves in a non-uniform background plasma
without recourse to the small-wavelength approximation. We show that the waves
undergo reflection near the reconnection current sheet due to the Alfv\'en
speed gradient and that the reflection efficiently depends on the
plasma-$\beta$ parameter as well as on the wave frequency. In particular, we
find that waves are reflected more efficiently near reconnection sites in a
low-$\beta$ plasma which is typical for the solar coronal conditions. Also, the
reflection is larger for lower frequency waves while high frequency waves
propagate outward from the reconnection region almost without the reflection.
We discuss the implications of efficient wave reflection near magnetic
reconnection sites in strongly magnetized coronal plasma for particle
acceleration, and also the effect this might have on First Ionization Potential
(FIP) fractionation by the ponderomotive force of these waves in the
chromosphere.
