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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…. - PowerPoint PPT Presentation

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  • ADIOS Revisited

    Mitch BegelmanJILA, University of Colorado

    ADIOS Revis it ed

  • ROGERS WRONGEST PAPER?Started: 1987 AAS, Pasadena

  • HOPEFULLY LESS WRONGStarted: 1998 AAS, San Diego

  • The ADIOS model addresses a fundamental problem in accretion theoryHOW DOES ROTATING GAS ACCRETE IF IT CANT RADIATE EFFICIENTLY?

  • ACCRETION REQUIRES TORQUE +TORQUE TRANSPORTS ENERGYTHE PROBLEM:

  • IN A THIN ACCRETION DISK:Local rate of energy release:

    Local rate of dissipation:2/3 of energy dissipated at R transported from

  • IN A RADIATIVELY INEFFICIENT ACCRETION FLOW:GEnergy transport from small R by torque unbinds gas at large R

  • ADIOS =Torque a conveyor belt for liberated energyFlow must find a way to limit energy transported outward from smaller r

    Mass loss or circulationSmall fraction of supplied mass reaches BHADIABATIC INFLOW-OUTFLOWSOLUTION (Blandford & Begelman 99)1 g of gas accreting at r ~ m can liberate 1 kg of gas at r ~ 1000 m

  • THE ADIOS MODEL

  • SELF-SIMILAR DISK WINDS Wind: Inviscid outflow with B < 0 Disk: Viscous flow with B < 0Jet: Evacuated coneEntropy increases at disk-wind interfaceHigh shear across windNo internal mixing across streamlinesHuge parameter space of solutionsBlandford & Begelman 2004

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

  • SELF-SIMILAR DISK WINDS Wind: Inviscid outflow with B < 0 Disk: Viscous flow with B < 0 Blandford & Begelman 2004Entropy increases at disk-wind interfaceHigh shear across windNo internal mixing across streamlinesHuge parameter space of solutions0
  • Hawley & Balbus 02SIMULATIONS SHOW MORE RESTRICTIVE BEHAVIOR...

  • Lindner, Milosavljevic, Couch, and Kumar 2009, preprint

  • Lindner, Milosavljevic, Couch, and Kumar 2009, preprint

  • TWO-ZONE ADIOS MODELMass Outflow Ang.Mom. Exchange: Mass Energy Ang. Mom.AVERAGE OVER STREAMLINESCONSERVE ENERGY, ANG. MOM. IN EACH ZONECONSERVE EXCHANGED ENERGY, ANG. MOM.

  • TWO-ZONE ADIOS MODELNO SOLUTION UNLESS:INCLUDE CENTRAL ENERGY SOURCE n 1TOTAL POWER AVAILABLE FRACTION DRIVES OUTFLOW, FLOWS THRU DISK

  • BREEZE MODELSBound, viscous inflowUnbound, very slow outflowViscous stress important in outflowThin disk limit, a=0Marginally bound inflowStress vanishes in outflowNo slow solution possible

  • BREEZE MODELSBound, viscous inflowUnbound, very slow outflowViscous stress important in outflow

  • WIND MODELSBound, viscous inflowUnbound, dynamical outflowViscous stress unimportant in outflow

  • WIND MODELSOUTFLOW CAN BE SUBSONIC OR SUPERSONIC BUT REQUIRES HIGH ENERGY INPUT ()SUBSONICSUPERSONIC

  • CONCLUSIONSA new type of ADIOS solutionwell-mixed outflowExplains ~R scalingInflow and outflow exchange M, L, but little EEnergy to drive outflow comes from centerTotal energy supply |Eacc|acc~/RFraction to outflow, 1- carried outward by inflowing gasDetails of inner accretion flow determine , Applications: SS433, Galactic Center

  • Started: 1987 AAS, PasadenaGestation period: 4 months

  • Started: 1998 AAS, San DiegoGestation period: 7 months

  • Started: 1998 Texas Symposium, ParisGestation period: 5 years

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

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