  The driving mechanism of massive outflows observed in high-mass star-forming
regions is investigated using three-dimensional magnetohydrodynamics (MHD) and
protostellar evolution calculations. In our previous paper, we showed that the
mass outflow rate depends strongly on the mass accretion rate onto the
circumstellar disk around a high-mass protostar, and massive outflows may be
driven by the magnetic effect in high-mass star-forming cores. In the present
study, in order to verify that the MHD disk wind is the primary driving
mechanism of massive outflows, we quantitatively compare outflow properties
obtained through simulations and observations. Since the outflows obtained
through simulations are slightly younger than those obtained through
observations, the time-integrated quantities of outflow mass, momentum, and
kinetic energy are slightly smaller than those obtained through observations.
On the other hand, time-derivative quantities of mass ejection rate, outflow
momentum flux, and kinetic luminosity obtained through simulations are in very
good agreement with those obtained through observations. This indicates that
the MHD disk wind greatly contributes to the massive outflow driving from
high-mass protostars, and the magnetic field might significantly control the
high-mass star formation process.
