1 / 17

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

Returning to the Source* MHD Disk Winds, Binaries and Jets as Agents of PN Shaping. Adam Frank University of Rochester F. Garcia-Arredondo, E. Blackman. Beyond the GISW. APNII 1999 – GISW can not recover many PN shapes.(*) Shaping begins during pPN stage.

paxton
Download Presentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Returning to the Source*MHD 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 • (T=105 K, L=5000 Lsol, r/h=10, ass = .1) • Md = 10-6 Msol/y

  8. MHD Disk Winds • Results for pPN Disks • (T=104 K, L=5000 Lsol, r/h=10, 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 < 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 Density Isosurfaces • Strong AGB/Jet Entrainment.

  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.

More Related