Geometry, Kinematics, and Magnetization of Simulated Prestellar Cores
  We utilize the more than 100 gravitationally-bound dense cores formed in our
three-dimensional, turbulent MHD simulations reported in Chen & Ostriker (2015)
to analyze structural, kinematic, and magnetic properties of prestellar cores.
Our statistical results disagree with the classical theory of star formation,
in which cores evolve to be oblate with magnetic field parallel to the minor
axes. Instead, we find that cores are generally triaxial, although the
core-scale magnetic field is still preferentially most parallel to the core's
minor axis and most perpendicular to the major axis. The internal and external
magnetic field directions are correlated, but the direction of integrated core
angular momentum is misaligned with the core's magnetic field, consistent with
recent observations. The ratio of rotational/total kinetic and
rotational/gravitational energies are independent of core size and consistent
in magnitude with observations. The specific angular momentum also follows the
observed relationship $L/M \propto R^{3/2}$, indicating rotation is acquired
from ambient turbulence. With typical $E_\mathrm{rot}/E_K \sim 0.1$, rotation
is not the dominant motion when cores collapse.
