  Very long baseline interferometry (VLBI) observations of SiO masers in Orion
Source I has enabled for the first time to resolve the outflow from a high-mass
protostar in the launch and collimation region. Therefore, Source I provides a
unique laboratory to study mass-loss and mass-accretion in a high-mass
protostar. We numerically simulate the dynamics of the disk-wind inside 100 AU
from Source I. This enables us to investigate the balance of different forces
(gravitational, magnetic, thermal) regulating gas dynamics in massive star
formation. In this work, we adopt magnetohydrodynamic (MHD) disk-wind models to
explain the observed properties of the disk-wind from Orion Source I. The
central source is assumed to be a binary composed of two 10\,$\msun$ stars in a
circular orbit with an orbital separation of 7 AU. High resolution ideal MHD
wind launching simulations (which prescribe disk as a boundary) are performed
using the PLUTO code. The simulations are allowed to run until a steady state
is obtained. MHD driven disk-wind provides a consistent model for the
wide-angle flow from Source I probed by SiO masers, reproducing the bipolar
morphology, the velocity amplitude and rotational profile, the physical
conditions, and the magnetic field strength.
