1 / 27

ADIOS Revisited

ADIOS Revisited. ed. ADIOS Revis. it. Mitch Begelman JILA, University of Colorado. Started: 1987 AAS, Pasadena. ROGER’S WRONGEST PAPER?. Started: 1998 AAS, San Diego. HOPEFULLY LESS WRONG. The ADIOS model addresses a fundamental problem in accretion theory….

hung
Download Presentation

ADIOS Revisited

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. ADIOS Revisited ed ADIOS Revis it Mitch Begelman JILA, University of Colorado

  2. Started: 1987 AAS, Pasadena ROGER’S WRONGEST PAPER?

  3. Started: 1998 AAS, San Diego HOPEFULLY LESS WRONG

  4. The ADIOS model addresses a fundamental problem in accretion theory… HOW DOES ROTATING GAS ACCRETE IF IT CAN’T RADIATE EFFICIENTLY?

  5. Angular Momentum Flux: G Energy Flux: THE PROBLEM: ACCRETION REQUIRES TORQUE +TORQUE TRANSPORTS ENERGY

  6. G IN A THIN ACCRETION DISK: Local rate of energy release: Local rate of dissipation: 2/3 of energy dissipated at R transported from <R by viscous torque

  7. Energy Transport: Bernoulli Function IN A RADIATIVELY INEFFICIENT ACCRETION FLOW: G Energy transport from small R by torque unbinds gas at large R

  8. ADIOS = 1 g of gas accreting at r ~ m can liberate 1 kg of gas at r ~ 1000 m • Torque a “conveyor belt” for liberated energy • Flow must find a way to limit energy transported outward from smaller r • Mass loss or circulation • Small fraction of supplied mass reaches BH ADIABATIC INFLOW-OUTFLOW SOLUTION (Blandford & Begelman 99)

  9. Ang.Mom. Energy Mass Energy Ang. Mom. Mass Outflow or circulation THE ADIOS MODEL

  10. SELF-SIMILAR DISK WINDS Disk:Viscous flow with B < 0 Entropy increases at disk-wind interface Wind:Inviscid outflow with B < 0 Jet:Evacuated cone High shear across wind No internal mixing across streamlines Huge parameter space of solutions Blandford & Begelman 2004

  11. SELF-SIMILAR DISK WINDS Disk:Viscous flow with B < 0 Entropy increases at disk-wind interface Wind:Inviscid outflow with B < 0 Blandford & Begelman 2004

  12. SELF-SIMILAR DISK WINDS Disk:Viscous flow with B < 0 Entropy increases at disk-wind interface Wind:Inviscid outflow with B < 0 High shear across wind No internal mixing across streamlines Huge parameter space of solutions 0<n<1 Blandford & Begelman 2004

  13. SIMULATIONS SHOW MORE RESTRICTIVE BEHAVIOR... Hawley & Balbus 02

  14. Lindner, Milosavljevic, Couch, and Kumar 2009, preprint

  15. Lindner, Milosavljevic, Couch, and Kumar 2009, preprint

  16. TWO-ZONE ADIOS MODEL Energy Ang.Mom. Exchange: Mass Energy Ang. Mom. Mass Outflow AVERAGE OVER STREAMLINES CONSERVE ENERGY, ANG. MOM. IN EACH ZONE CONSERVE EXCHANGED ENERGY, ANG. MOM.

  17. TWO-ZONE ADIOS MODEL CENTRAL ACCRETION ENERGY DRIVES OUTFLOW Ang.Mom. Energy Exchange: Mass Energy Ang. Mom. Mass Outflow NO SOLUTION UNLESS: INCLUDE CENTRAL ENERGY SOURCE n ≈ 1 TOTAL POWER AVAILABLE FRACTION DRIVES OUTFLOW, FLOWS THRU DISK

  18. BREEZE MODELS Bound, viscous inflow Unbound, very slow outflow Viscous stress important in outflow No slow solution possible Thin disk limit, a=0 Stress vanishes in outflow Marginally bound inflow

  19. BREEZE MODELS Bound, viscous inflow Unbound, very slow outflow Viscous stress important in outflow

  20. WIND MODELS Bound, viscous inflow Unbound, dynamical outflow Viscous stress unimportant in outflow

  21. WIND MODELS OUTFLOW CAN BE SUBSONIC OR SUPERSONIC … BUT REQUIRES HIGH ENERGY INPUT () SUPERSONIC SUBSONIC

  22. CONCLUSIONS • A new type of ADIOS solution • “well-mixed” outflow • Explains Ṁ~R scaling • Inflow and outflow exchange M, L, but little E • Energy to drive outflow comes from center • Total energy supply |Eacc|Ṁacc~Ṁ/R • Fraction  to outflow, 1- carried outward by inflowing gas • Details of inner accretion flow determine ,  • Applications: SS433, Galactic Center …

  23. Started: 1987 AAS, Pasadena Gestation period: 4 months

  24. Started: 1998 AAS, San Diego Gestation period: 7 months

  25. Started: 1998 Texas Symposium, Paris Gestation period: 5 years

  26. Started: 1999 KITP BH Meeting, Santa Barbara Gestation period: 8 years

  27. Started: 2009 BlandfordFest, Stanford Gestation period: ?? arXiv:??10.2327v1 [astro-ph.HE] 17 Oct 20??

More Related