YSO Jets: Feedback from Mesoscopic to Macroscopic scales Adam Frank University of Rochester Andrew Cunningham, Kris Yirak Eric Blackman, Alice Quillen, Sorin Mitran (UNC), John Bally (CU), Pat Hartigan (Rice)

The Tool: AstroBEAR AMR Code Cunningham, Frank, Varniere & Mitran 2007* “Block” AMR Choice of solvers/integrators Parallel – load balance Multi-physics modules: Ionization and H2Chemistry heat conduction *self-gravity *rad trans (diff limit) MHD Flux conservation via CT

Radiative Outflows in Heterogeneous Media Cunningham, Frank, Varniere & Mitran 2007*

Feedback on Meso & Maco Scales. Microscopic = launch region (L < 100 AU) Mesoscopic = Individual outflow (L < .1 pc) Macroscopic = Cluster/pc-scale flow ( L ~ 1 pc) Mesoscopic Outflow’s affect on “envelope”: density velocity emission

Scattered Light Cavities Laski, Frank, Cunningham 2007* Explore envelope shaping via: Jets Wide Angle Winds Envelope: rotating collapse. Use scattered-light code for images Wood et al… Shang et al. 2006 10000 au

Macroscopic Scales: Outflow Feedback & Turbulence Can space-filling isotropic turbulence be driven by needles (jets), or balloons (outflows)? Explicate mechanisms. Connection with observational structures. Global Analytics – Matzner, Tan, Krumhotz, others Global sims – Maclow 2000, Nakamura & Li 2005, 2007 Resolution critical for jet sims : Rj ~ 20 zones. Observation: total outflow energy budgets = cloud/cluster turbulent energy (Walawender et al 2006, Sandell & Knee 2001). Observation: Parsec outflows common (Bally, Devine Reipurth, Ray) Typical cloud size/stellar density => whole cluster overrun by outflows. Tens/Hundreds proto-stars eject enough Ek replenish Eturb.

Project 1: Outflow Collisions as a Route to Turbulence Explore effect of single collisions on accelerating ambient material. Vary impact parameter b Cunningham, Frank & Blackman 2006

Collisions reduce effective “entrainment” Increase Radiative Losses Results b = 0 b = rj b = 5.3 rj b=0 b=rj b=5rj Collisions reduce effective “entrainment” Increase Radiative Losses Bad for turbulence. b=0 b=rj b=5rj

Project 2: Fossil Cavities as Intermediaries to Protostellar Turbulence Observations of NGC 1333 : Quillen et al 2005 Simulations of Fossil Cavities Cunningham et al 2006

Project 2: NGC 1333: A Test Case (Quillen et al 2005) NGC 1333: Numerous active outflows (Knee & Sandell 2000 Walsh et. al 2006) Explore High Rez 13CO Data - No correlation of outflows with velocity dispersion. (Ridge et al, COMPLETE) But…numerous low V cavities seen in channel maps. No stellar source at center of cavities – Fossil Cavities of extinct outflows. Scaling relation: Ek(fossil outflows) ~ Eturb

Cavity Simulations Cunningham, Frank, Blackman & Quillen 2006 Explore time-decaying Jets/WAW outflow evolution (Bertout et al 96) Outflow power decays after 104 y. Simulation runs for 105 y Run to 0.5 pc scales Compare with scaling relations of Quillen et al. Compare with PV diagrams

Fossil Cavity Sims: Jets and WAW Collimated Jet Wide Angle Wind (Matzner Class Sol) Strong deceleration Rarefactions backfill cavity

Fossil Cavity Sims: Results Quillen et al scaling relation for momentum Simulation comparison: deviation from scaling relation small jets WAW Time dependent jets/wind = fossil cavities = turbulent support

Project 3: Radiative Jets in Turbulent Media Mechanism for a single jet Cunningham et al. 2007*

Time-dependent Jets in Turbulent Environment Long Period 2-D slices of 3-D simulation Short Period

Time Dependent Jets in a Turbulent Environment Intermediate pulse Long pulse Without jet, turbulence decays as expected. With jet, “turbulence” re-energized on all scales. With jet long “driving” scales energized which not previously present.

Future: Focus on Individual Objects L1551 Frank, Bally, Blackman, Hartigan 200x

“Region” between Meso-scale and Macro-scale likely to matter. Conclusions Colliding Jets Interactions of active outflows not important. NGC 1333/Fossil Cavities Fossil cavities “store” momentum. Fossil cavities = transient jets/outflows Momentum budgets match Outflows in Turbulent Media Outflows re-energize turbulence. “Region” between Meso-scale and Macro-scale likely to matter.