  We present ALMA images of the dust and molecular line emission in the Orion
Hot Core at 349 GHz. At 0.2" angular resolution the images reveal multiple
clumps in an arc ~ 1" east of Orion Source I, the protostar at the center of
the Kleinmann-Low Nebula, and another chain of peaks from IRc7 towards the
southwest. The molecular line images show narrow filamentary structures at
velocities > 10 km/s away from the heavily resolved ambient cloud velocity ~5
km/s. Many of these filaments trace the SiO outflow from Source I, and lie
along the edges of the dust emission. Molecular line emission at excitation
temperatures 300--2000 K, and velocities > 10 km/s from the ambient cloud,
suggest that the Hot Core may be heated in shocks by the outflow from Source I
or from the BN/Source I explosion. The spectral line observations also reveal a
remarkable molecular ring, ~ 2" south of Source I, with a diameter ~ 600 AU.
The ring is seen in high excitation transitions of HC3N, HCN v2=1, and SO2. An
impact of ejecta from the BN/Source I explosion with a dense dust clump could
result in the observed ring of shocked material.
