[Previous] | [Session 57] | [Next]
C.-F. Lee, J. Stone, E. Ostriker, L. Mundy (UMD)
We present simple steady jet and wind simulations to explain the observed properties of CO molecular outflows associated with young low-mass stars. In the simulations, jet/wind is allowed to propagate into a stratified ambient material and sweep up the ambient material into a thin swept-up shell seen as the molecular outflow. A simple impulse model is used to interpret the structure and kinematics of the swept-up shell in the jet simulations, while a momentum-driven shell model is used to explain the structure and kinematics of the swept-up shell in the wind simulations. We calculate position-velocity (PV) diagrams cut along the major axis and mass-velocity (MV) relationships for the shell material, allowing direct comparing of the simulations with the observations. In the jet simulations, the jet-driven bow shock is associated with a broad range of velocities, producing the convex spur PV structures in the observations. In the wind simulations, the velocity of the shell material is more radially directed than that in the jet simulations, producing the parabolic PV structures in the observations. The power-law index of the mass-velocity relationships is between 1.5 and 3.5 for the jet-driven shell, and between 1.3 and 1.8 for the wind-driven shell in the simulations.
The author(s) of this abstract have provided an email address for comments about the abstract: chinfei@astro.umd.edu