YSO Jets: Feedback from Mesoscopic to Macroscopic scales - PowerPoint PPT Presentation

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YSO Jets: Feedback from Mesoscopic to Macroscopic scales

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  1. 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)

  2. 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

  3. Radiative Outflows in Heterogeneous MediaCunningham, Frank, Varniere & Mitran 2007*

  4. 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

  5. Scattered Light CavitiesLaski, 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

  6. 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.

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

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

  9. Project 2:Fossil Cavities as Intermediaries to Protostellar TurbulenceObservations of NGC 1333 : Quillen et al 2005Simulations of Fossil CavitiesCunningham et al 2006

  10. 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

  11. Cavity SimulationsCunningham, 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

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

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

  14. Project 3:Radiative Jets in Turbulent MediaMechanism for a single jetCunningham et al. 2007*

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

  16. 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.

  17. Future: Focus on Individual ObjectsL1551Frank, Bally, Blackman, Hartigan 200x

  18. 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.