Simulations parameters Numerical Simulations Velocity Distribution

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Presentation transcript:

Simulations parameters Numerical Simulations Velocity Distribution The Dynamics of Protostellar Outflow Interactions J. Carroll1, A. Frank1, E. Blackman1 1 University of Rochester, Rochester, NY Outflow Properties Abstract Simulations parameters Vshell l ρ I ρ 371 M☼ /pc3 I 17 M☼ /Myr S 59 pc-3Myr -1 l .36 pc t .36 Myr m 17 M☼ cs .2 km/s ρoutflow 92 M☼ /pc3 voutflow 240 km/s toutflow .8 kyr θhalf 5° routflow .03 pc Protostellar outflows and their cavities are commonly observed within turbulent molecular cloud cores. However, the interplay between cloud turbulence and protostellar outflows remains poorly understood. Recent simulations of star forming cloud cores demonstrate that outflows can be important in regulating the SFR. Here we investigate the ability of many outflow interactions to seed turbulence and attempt to characterize the length scale at which outflows become subsumed into the overall turbulence. Numerical Simulations Velocity Distribution Conclusions Collimated protostellar outflows are able to drive supersonic turbulent motions in molecular cloud cores at velocities consistent with theoretical predictions… and necessary to provide turbulent support against core collapse. The energy spectra associated with outflow driven turbulence indicates an outflow driving scale consistent with theoretical predictions… Hydrodynamic simulations were performed on a periodic cube of length 1.5 pc for 1 Myr at a resolution of 2563 using a polytropic equation of state (γ=1.0001) to approximate an isothermal gas at 10°K Spectra Density Distribution Acknowledgements