Returning to the Source MHD Disk Winds, Binaries and Jets as Agents of PN Shaping - PowerPoint PPT Presentation

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Returning to the Source MHD Disk Winds, Binaries and Jets as Agents of PN Shaping

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Momentum Deficits (Burjarrabal 01) If this bears out may be THE critical ... No corkscrew. Spiral shocks and High density at midplane. Strong Jet Case: c = .63 ... – PowerPoint PPT presentation

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Title: Returning to the Source MHD Disk Winds, Binaries and Jets as Agents of PN Shaping


1
Returning to the SourceMHD Disk Winds, Binaries
and Jets as Agents of PN Shaping
  • Adam Frank
  • University of Rochester
  • F. Garcia-Arredondo, E. Blackman

2
Beyond the GISW
  • APNII 1999
  • GISW can not recover many PN shapes.()
  • Shaping begins during pPN stage.
  • Momentum Deficits (Burjarrabal 01)
  • If this bears out may be THE critical result for
    us!

3
MHD Wind Launching
  • 2 Versions of Models
  • Rapidly Rotating Magnetized Core
  • (no binary needed)
  • Blackman et al Nature 2001
  • Matt, Blackman Frank 2003
  • Magnetized Accretion Disk
  • (need binary)
  • Blackman, Frank Welch 2001
  • Disk forms around primary (Companion disrupted)
  • (Soker, Livio, Reyes-Ruiz, Lopez)
  • Disk forms around companion (Soker, Livio etc)

4
MHD Disk Winds
  • Soker Livio (1994) say Disk Jet.
  • For PNe conditions this requires Strong Magnetic
    Field!
  • Fast Magnetic Rotator (Not Chevalier Luo 1994
    Models)
  • Can we apply MHD Disk Wind Theory to PNe type
    accretion disks?

5
MHD Disk Winds Frank Blackman 2003
  • Begin with disk parameters (Acc. Rate etc.)
  • Step 1 Steady Axisymmetric MHD Eq.
  • Disk radius r0, disk height h, Rotation W0
  • Step 2 Derive Alfven Radius rA
  • Step 3 Derive Uinf and Mass Loss Rate
  • Step 4 Derive BA from dynamo (ass)

6
MHD Disk Winds Results
7
MHD Disk Winds
  • Results for PN Disks
  • (T105 K, L5000 Lsol, r/h10, ass .1)
  • Md 10-6 Msol/y

8
MHD Disk Winds
  • Results for pPN Disks
  • (T104 K, L5000 Lsol, r/h10, ass .1)
  • Md 10-4 Msol/y

9
MHD Disk Winds
  • Use Reyes-Ruiz Lopez 99 disk model.
  • Recover pPN Momentum and Energy.

10
Jets in Binary Systems (Garcia-Arredondo Frank
2003)
  • Jets or Collimated Fast Winds (CFW) from orbiting
    companion must propagte through expanding AGB
    wind
  • Soker Rapport 2000, Livio Soker 2002
  • Goal Explore flow pattern within 400 AU of
    source.
  • Requires AMR (Yaguzua, Raga et al 2000)

11
Deflection and Disruption
Key parameter ratio of momentum between AGB wind
and Jet
Use isothermal EOS c .63, 5 a 10o
12
Strong Jet Case c .625
  • Flow bounded by U or V shaped shocks in AGB wind
  • Tcross lt Torb. No corkscrew.
  • Spiral shocks and High density at midplane

13
Strong Jet Case c .63
  • Strong AGB/Jet Entrainment.

14
Weak Jet Case c 5
  • Flow bounded by U or V shaped shocks in AGB wind
  • Significant bending and disruption (Sideways
    shocks)
  • Complex flow pattern (Donkey Ear Shells)

15
Weak Jet Case c 5
  • Strong AGB/Jet Entrainment.

16
Weak Jet Case c 5
  • Strong AGB/Jet Entrainment.

Density Isosurfaces
17
Conclusions
  • MHD Disk Winds can power PN
  • MHD Disk Winds can power high momentum pPN (
    need high acc. rate)
  • CFW/AGB interaction complex but promising.
  • Need more numerical exploration of binary
    scenarios.
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