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The proper motions of the three stars ejected from Orion's OMC1 cloud coreare combined with the requirement that their center of mass is gravitationallybound to OMC1 to show that radio source I (Src I) is likely to have a massaround 15 Solar masses consistent with recent measurements. Src I, the starwith the smallest proper motion, is suspected to be either an AU-scale binaryor a protostellar merger remnant produced by a dynamic interaction ~550 yearsago. Near-infrared 2.2 um images spanning ~21 years confirm the ~55 km/s motionof `source x' (Src x) away from the site of stellar ejection and point oforigin of the explosive OMC1 protostellar outflow. The radial velocities andmasses of the Becklin-Neugebauer (BN) object and Src I constrain the radialvelocity of Src x to be V_{LSR} = -28 +/-10 km/s . Several high proper-motionradio sources near BN, including Zapata 11 ([ZRK2004] 11) and a diffuse sourcenear IRc 23, may trace a slow bipolar outflow from BN. The massive disk aroundSrc I is likely the surviving portion of a disk that existed prior to thestellar ejection. Though highly perturbed, shocked, and re-oriented by theN-body interaction, enough time has elapsed to allow the disk to relax with itsspin axis roughly orthogonal to the proper motion.

The Orion Protostellar Explosion and Runaway Stars Revisited: Stellar Masses, Disk Retention, and an Outflow from BN