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

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

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

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

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

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

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

8. 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 ADIOS = ADIABATIC INFLOW-OUTFLOW SOLUTION (Blandford & Begelman 99) 1 g of gas accreting at r ~ m can liberate 1 kg of gas at r ~ 1000 m

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

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

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

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

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

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

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

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

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

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 (  ) SUBSONIC SUPERSONIC

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 acc –Total energy supply |E acc | Ṁ acc ~  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??