Protostellar Outflows, Feedback and Turbulence Looking to HEDLA 9

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Protostellar Outflows, Feedback and
TurbulenceLooking to HEDLA 9

• Adam Frank
• University of Rochester
• Andrew Cunningham, Peggy Varniere, Eric Blackman,
  Alice Quillen

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HEDLA Jet Studies Maturing Compare with HEDLA 3
(1998)
Lasers (UR LLE)
Pulsed Power
3
What Next?

• Most stars form jets or bipolar outflows
• Stars do not form in isolation.
• Explore Outflow-Outflow Interactions
• Why?

Feedback on Large Scales Turbulence
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Outflows Interactions? (Bally et al)

• Orion Nebula
• 1000 stars/pc3
• (Bally et al..)

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Turbulence and Molecular Clouds Perseus

• M 104 Mo, D 8x25 pc
• Vturb 2 10 km/s Gradient east to west

13CO map Perseus Molecular Cloud O HH
objects Walender et al 2005
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The Problem Turbulent Decay

• Turbulence needed to maintain pressure support
  for molecular clouds.
• Without continued energy injection (HD or MHD)
  turbulence decays rapidly (Stone, Ostriker,
  Maclow)
• tdecay lt tcollapse

Kinetic energy vs time for 4 decaying turbulent
sims (MacLow 02 Hydro, MHD, ZUES, SPH)
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Protostellar Turbulence

• Observation total outflow energy budgets cloud
  turbulent energy
• Observation Parsec outflows common
• Volume fill ratio
• L1 pc, Rbs0.1 pc, N32 pc-3 gt
• 32 protostars pc-3 whole cloud or core overrun
  by outflows.
• Tens/Hundreds proto-stars eject enough Ek
  replenish Eturb

• Can space-filling isotropic turbulence be driven
  by sticking needles, (balloons) into molecular
  clouds?

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Project 1Outflow Collisions as a Route to
TurbulenceExplore effect of single collisions
on accelerating ambient material. (Jet)2, (Wide
Angle Wind) 2. Vary impact parameter b
Cunningham, Frank Blackman 2006
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The ToolAstroBEAR AMR Code

• Block AMR Retain grids upon refinement
  (Burger Collella)
• Set of Riemann solvers (Full, Roe, MHD).
• Parallel load balance and domain decomposition
• Built-in physics modules
• Time-dependent Ionization and H2Chemistry
• heat conduction (multi-grid)
• self-gravity
• rad trans (diff limit)
• MHD Flux conservation via CT
• AMR MHD jet sims
• Hartigan et al (in prep)

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Results
b5rj
brj
b0
b0
brj
b5rj
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Jet-Jet Collisions Case A
Impact Parameter b 0 Volume Rendering
of Density with 2-D slice at mid-plane
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Jet-Jet Collisions Cases B C
Impact Parameter b rj
Impact Parameter b 5.33 rj
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M vs V Plots

• RESULTS
• For jets we find n 1.7
• Little difference between interacting (b 0, rj)
  and non-interacting cases (b gtgt rj)!
• Surface Area Effect 2 jets become 1

• M(v) or dP/dv diagnostic for molecular outflows
• Power law for low velocities.

Collisions reduce effective entrainment Increase
Radiative Losses Bad for turbulence.
Jet
WAJ
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Project 2Fossil Cavities as Intermediaries to
Protostellar TurbulenceObservations of NGC 1333
Quillen et al 2005Simulations of Fossil
CavitiesCunningham et al 2006
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Project 2 NGC 1333 A Test Case(Quillen et al
2005)

• NGC 1333 Numerous active outflows
• Explore High Rez 13CO Data - No correlatation of
  outflows with velocity dispersion
• Butnumerous low V cavities seen in channel
  maps.
• No stellar source at center of cavities Fossil
  Cavities of extinct outflows.
• In Fossil Cavities
• Ek(outflow) Eturb

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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
  2005
• Compare with PV diagrams

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Fossil Cavity Sims Jets and WAW
Collimated Jet
Wide Angle Wind (Matzner Class Sol)

• Strong deceleration
• Rarefactions backfill cavity

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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
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Project 3 Jets in a Turbulent EnvironmentCunning
ham Frank Blackman (in progress)
2-D slice of 3-D simulation
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Conclusions

• Colliding Jets
• Interactions of Active Jets may not matter
• Look at time and space domain
• NGC 1333/Fossil Cavities
• Active jets do not couple well to cloud
• Fossil cavities store momentum
• Energy and Momentum budgets OK
• Fossil cavities well represented by transient
  jets
• Lab Astro Signifigant progress in jets/outflows
• Can we do outflow interaction experiments?

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AstroBEAR with Heat Condution
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Table of Contents

• Intro Jets, Clusters and Turbulence
• A Numerical Interlude AstroBEAR.
• Parallel MHD AMR
• Study 1 Colliding 3-D Outflows
• Study 2 Fossil Outflow Cavities
• The Case of NGC 1333
• Fossil Cavity Simulations
• Study 3, 4, 5 Works in Progress
• Conclusions

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Giant Molecular Clouds
The Raw Material of Star and Planet Formation

• Massive M 103 to 106 x MSun
• Molecular H2
  (70)
• He
  (29)
• Trace Molecules
  (1)
• CO, OH, CS, HCO,
• organics, ,
  
• Cold T 5 to 50 K
• Dense n(H2) 100 to gt 105 cm-3
• Giant L 10 to 100 light
  years

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Feedback on Large Scales Turbulence

• What is Turbulence? (Scalo Elmegreen 04)
• Turbulence is non-linear fluid motion resulting
  in the excitation of an extreme range of
  correlated spatial and temporal scales. There is
  no clear scale separation for a perturbation
  expansion and the number of degrees of freedom is
  too large to treat as chaotic and too small to
  treat in a statistical mechanics sense
• Kolmogorov Scalings Energy injected at large
  scale cascades to small dissipational scales

Energy per unit mass per unit wavelength
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Turbulence in Clouds

• ISM Turbulent.
• Molecular Clouds are Turbulent (!?!).
• Larson (1981) power-law correlation between
  cloud size and line widths (like Kolmogorov
  scalings).

12CO emission of outer galaxy Heyer et al 98
Integrated HI emission from LMC Elmegreen et al 01
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The Problem Turbulent Decay

• Turbulence needed to maintain pressure support
  for molecular clouds.
• Without continued energy injection (HD or MHD)
  turbulence decays rapidly (Stone, Ostriker,
  Maclow)
• tdecay lt tcollapse

Kinetic energy vs time for 4 decaying turbulent
sims (MacLow 02 Hydro, MHD, ZUES, SPH)
31
Sources of Turbulence in Clouds

• Turbulence will not delay collapse.
• How to maintain Eturb?
• What is energy source?
• Are clouds long lived?
• Sources of Turbulence
• SNe
• Gravitational Collapse
• HII Regions
• Galactic Rotation
• Protostellar Outflows

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Hypersonic Swizzle Sticks.Can Outflows Power
Turbulence?

• Idea of Self-regulation goes back at least to
  Norman Silk 1980
• Outflows generally thought to contain enough
  energy to drive turbulence
• Yes Bally et al 96, Knee Sandell 00
• Arce Goodman
• No Walwander et al 05
• As yet, no detailed theoretical studies of link
  between outflows and turbulence

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Jets vs. Molecular OutflowsJets vs. Wide Angle
Winds (WAWs)
HH Jet HH 111
Molecular Outflow IRAS 16316
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Study 1 Jet Interactions

• Jets are spikes in momentum space?
• Momentum input bounded by shocks Prompt
  Entrainment
• How to convert jet energy/momentum into
  turbulence?
• Jet collisions?
• For parsec scale outflows filling factor of 10
  or more

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Jet/Outflow InteractionsCunningham, Frank
Blackman 06

• 3-D AMR Hydro simulations with time-dependent
  cooling.
• Explore quantitative measures of stirring
• (M vs V), Pamb/Ptotal, Vorticity
• Allow collimated jets or wide angle jets (WAJs q
  15o) to collide at w 90o

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Jet-Jet Collisions Case A
Impact Parameter b 0 Volume Rendering
of Density with 2-D slice at mid-plane
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Jet-Jet Collisions Cases B C
Impact Parameter b rj
Impact Parameter b 5.33 rj
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WAJ-WAJ Collisions Case A
Impact Parameter b 0 Volume Rendering
of Density
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WAJ-WAJ Collisions Cases B C
Impact Parameter b rj
Impact Parameter b 5.33 rj
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M vs V Plots

• RESULTS
• For jets we find n 1.7
• Little difference between interacting (b 0, rj)
  and non-interacting cases (b gtgt rj)!
• Surface Area Effect 2 jets become 1

• M(v) or dP/dv diagnostic for molecular outflows
• Power law for low velocities.

Jet
WAJ
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Vorticity Injection

• Total Vorticity in Computational Space
• Power Law W(t) Wotn, 0ltnlt1
• Suppress W(t) after collision.

Surface Area Effect 2 jets become 1
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Study 1Conclusions

• Direct Collisons produce dramatic changes in
  morphology
• 2 jets become 1
• No dramatic change in quantitative measures.
• M(v), camb(t), W(t)
• Changes are negative collisions less
  effective at accelerating/stirring ambient gas
• Result appears to be surface area effect reduce
  surface area over which prompt entrainment occurs

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The Real Thing NGC 1333

• Reflection nebula associated with Perseus
  Molecular Cloud
• Perseus Cloud M 104 Mo, D 8x25 pc
• No high mass stars forming now (10 Myr ago?)
• Vturb 2 10 km/s Gradient east to west

13CO low rez map Perseus Molecular Cloud O HH
objects Walender et al 2005
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NGC 1333 in Perseus 150 young stars
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NGC 1333 A Test Case(Quillen et al 2005)

• NGC 1333 Actually 2 Young Star Clusters
• Claim 1 Energy to power cloud/cluster turbulence
  exits in current outflow activity (Aspen et al
  03, Knee Sandell 00)
• Claim 2 Not enough energy to power cloud
  turbulence in current outflow activity
  (Walawender et al 05)

13CO map Westeren edge Per. Cloud HH
objects. NGC 1333 top center Walender et al 2005
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NGC 1333 Data

• Explore High Rez 13CO Data (Ridge et al 04)
• Correlate with Spitzer images 2Mass data etc.

13CO map Spitzer 4.5 m image CO Data .2 km/s
contour spacing .47 km/s gradient top to
bottom Spitzer data SVS13 center left Many
outflows visible
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NGC 1333 Cavities

• No significant structure correlated with know
  outflows seen velocity dispersion in 13CO data
  (Vdisp 1 km/s)
• Bulk of cloud (traced by 13CO) no high V gas
  associated with active outflows
• Butnumerous low V cavities seen in channel maps.
• Cavities appear in neighboring channels
• Different cavities not in same channels.
• i.e. Cavities are real

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NGC 1333 PV Diagrams/Properties

• Limb-Brightened Shells or Shell Fragments
• Expansion Velocities of Vexp 1. km/s
• Vexp 3 Vturb
• Lcav .1 - .5 pc (cross section)
• texp 5x105 106 y

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NGC 1333 Global Properties

• 22 Cavities in 1x1pc region
• 10 volume filling fraction
• Ncav Lower limit lower
• Lower Vexp or lower density contrast (2 -3)
  would be missed.
• Cavities NOT associated with stars (2Mass
  database)
• tbackfill Lcav/c few x 105 y

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NGC 1333 Global Energetics

• Simple Model Cylindrical Wind Blown Bubble

• Knee and Sandell 00 total momentum in 6 active
  (12CO) outflows flows 10 Mo km/s
• Typical individual outflow .2 2 Mo km/s
• Our outflows show similar momentum has been
  coupled to cloud.
• Turbulence
• Cavity Energy Injection Rate dE/dt 4 x 1032
  erg/s
• Turbulent Dissipation Rate
  1033 erg/s

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Cavity SimulationsCunningham Frank Blackman
Quillen 2006

• Explore Long Lived Jets/WAW outflow interactions.
• Outflow power decays after 10000 y.
• Simulation runs for 100,000 y
• Run to 0.5 pc scales
• Compare with PV diagrams

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Fossil Cavity Sims Jets

• Rarefaction runs laterally
• Jet head shows deceleration

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Fossil Cavity Sims Wide Angle Wind (Matzner
Class Sol)

• Wider outflow Generated
• Strong deceleration

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Lab Astro Laser JetsWilliams et al 2005

• UR Omega Laser
• M 4 jets and bow shocks

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Lab Astro Laser JetsSublett, Knauer et al 2006

• UR Omega Laser
• Pulsed Jets and Bow Shocks
• Decaying Jets!

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Laboratory MHD Jet ExperimentsLededev, Frank,
Blackman et al 2005

• Can now make B dominated flow in Lab!
• MAGPIE Pulsed Power machine 16 wire radial
  array.
• Global Bf below wire
• Wires ablate plasma atmosphere
• Wires break Bf inflates magnetic outflow and
  collimates axial jet

Simulation
Experiment Soft X-ray Images
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Future Direction Turbulent Environment
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Conclusions

• Colliding Jets
• Interactions of Active Jets may not matter
• Look at time and space domain
• NGC 1333
• Active jets do not couple well to cloud
• Fossil cavities store momentum
• Energy and Momentum budgets OK
• Fossil cavities well represented by transient
  jets
• Ongoing Feedback on smaller scales scattered
  light cavities
• Lab Astro Signifigant progress in jets/outflows

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Results Radiative Loss

• Shock jump relations - 20 of energy budget
  radiated by ambient material intercepted by the
  mach disk (for a single jet).
• Collimated jet collisions double radiative
  loss.
• Less energy available to drive turbulent motions
  once the driving source has ceased and the flow
  becomes subsumed into the cloud.