  I discuss different theories of massive star formation: formation from
massive cores, competitive Bondi-Hoyle accretion, and protostellar collisions.
I summarize basic features of the Turbulent Core Model (TCM). I then introduce
the Orion Kleinmann-Low (KL) region, embedded in the Orion Nebula Cluster (ONC)
and one of the nearest regions of massive star formation. The KL region
contains three principal radio sources, known as "I", "n" and "BN". BN is known
to be a runaway star, almost certainly set in motion by dynamical ejection
within the ONC from a multiple system of massive stars, that would leave behind
a recoiling, hard, massive, probably eccentric binary. I review the debate
about whether this binary is Theta^1C, the most massive star in the ONC, or
source "I", and argue that it is most likely to be Theta^1C, since this is now
known be a recoiling, hard, massive, eccentric binary, with properties that
satisfy the energy and momentum constraints implied by BN's motion. Source "n"
is a relatively low-mass protostar with extended radio emission suggestive of a
bipolar outflow. Source "I", located near the center of the main gas
concentration in the region, the Orion Hot Core, is the likely location of a
massive protostar that is powering the KL region, and I discuss how its basic
properties are consistent with predictions from the TCM. In this scenario, the
radio emission from source "I" is the base of a bipolar outflow that is ionized
by the massive protostar and should be elongated along the axis of the outflow.
