  We present sensitive high angular resolution submillimeter and millimeter
observations of torsionally/vibrationally highly excited lines of the CH$_3$OH,
HC$_3$N, SO$_2$, and CH$_3$CN molecules and of the continuum emission at 870
and 1300 $\mu$m from the Orion KL region, made with the Submillimeter Array
(SMA). These observations plus recent SMA CO J=3-2 and J=2-1 imaging of the
explosive flow originating in this region, which is related to the
non-hierarchical disintegration of a massive young stellar system, suggest that
the molecular Orion "Hot Core" is a pre-existing density enhancement heated
from the outside by the explosive event -- unlike in other hot cores we do not
find any self-luminous submillimeter, radio or infrared source embedded in the
hot molecular gas. Indeed, we do not observe filamentary CO flow structures or
"fingers" in the shadow of the hot core pointing away from the explosion
center. The low-excitation CH$_3$CN emission shows the typical molecular
heart-shaped structure, traditionally named the Hot Core, and is centered close
to the dynamical origin of the explosion. The highest excitation CH$_3$CN lines
are all arising from the northeast lobe of the heart-shaped structure, {\it i.
e.} from the densest and most highly obscured parts of the Extended Ridge. The
torsionally excited CH$_3$OH and vibrationally excited HC$_3$N lines appear to
form a shell around the strongest submillimeter continuum source. Surprisingly
the kinematics of the Hot Core and Compact Ridge regions as traced by CH$_3$CN
and HC$_3$N also reveal filament-like structures that emerge from the dynamical
origin. All of these observations suggest the southeast and southwest sectors
of the explosive flow to have impinged on a pre-existing very dense part of the
Extended Ridge, thus creating the bright Orion KL Hot Core.
