  We explore kinematics and morphologies of molecular outflows driven by young
protostars using magnetohydrodynamic simulations in the context of the unified
wind model of Shang et al. The model explains the observed high-velocity jet
and low-velocity shell features. In this work we investigate how these
characteristics are affected by the underlying temperature and magnetic field
strength. We study the problem of a warm wind running into a cold ambient
toroid by using a tracer field that keeps track of the wind material. While an
isothermal equation of state is adopted, the effective temperature is
determined locally based on the wind mass fraction. In the unified wind model,
the density of the wind is cylindrically stratified and highly concentrated
toward the outflow axis. Our simulations show that for a sufficiently
magnetized wind, the jet identity can be well maintained even at high
temperatures. However, for a high temperature wind with low magnetization, the
thermal pressure of the wind gas can drive material away from the axis, making
the jet less collimated as it propagates. We also study the role of the
poloidal magnetic field of the toroid. It is shown that the wind-ambient
interface becomes more resistant to corrugation when the poloidal field is
present, and the poloidal field that bunches up within the toroid prevents the
swept-up material from being compressed into a thin layer. This suggests that
the ambient poloidal field may play a role in producing a smoother and thicker
swept-up shell structure in the molecular outflow.
