ADIOS Revisited

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ADIOS Revisited
ed
ADIOS Revis
it

• Mitch Begelman
• JILA, University of Colorado

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Started 1987 AAS, Pasadena
ROGERS WRONGEST PAPER?
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Started 1998 AAS, San Diego
HOPEFULLY LESS WRONG
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The ADIOS model addresses a fundamental problem
in accretion theory
HOW DOES ROTATING GAS ACCRETE IF IT CANT RADIATE
EFFICIENTLY?
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ACCRETION REQUIRES TORQUE TORQUE TRANSPORTS
ENERGY
THE PROBLEM
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IN A THIN ACCRETION DISK
Local rate of energy release Local rate of
dissipation
2/3 of energy dissipated at R transported from ltR
by viscous torque
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IN A RADIATIVELY INEFFICIENT ACCRETION FLOW
G
Energy transport from small R by torque unbinds
gas at large R
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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)
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THE ADIOS MODEL
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SELF-SIMILAR DISK WINDS
Disk Viscous flow with B lt 0
Entropy increases at disk-wind interface
Wind Inviscid outflow with B lt 0
Jet Evacuated cone

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


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


High shear across wind No internal mixing across
streamlines Huge parameter space of
solutions 0ltnlt1
Blandford Begelman 2004
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SIMULATIONS SHOW MORE RESTRICTIVE BEHAVIOR...
Hawley Balbus 02
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Lindner, Milosavljevic, Couch, and Kumar 2009,
preprint
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Lindner, Milosavljevic, Couch, and Kumar 2009,
preprint
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TWO-ZONE ADIOS MODEL
Ang.Mom.
Exchange Mass Energy Ang. Mom.
Mass Outflow

AVERAGE OVER STREAMLINES CONSERVE ENERGY, ANG.
MOM. IN EACH ZONE CONSERVE EXCHANGED ENERGY, ANG.
MOM.
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TWO-ZONE ADIOS MODEL
NO SOLUTION UNLESS INCLUDE CENTRAL ENERGY SOURCE
n 1 TOTAL POWER AVAILABLE FRACTION
DRIVES OUTFLOW, FLOWS THRU DISK
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BREEZE MODELS
Bound, viscous inflow Unbound, very slow
outflow Viscous stress important in outflow
No slow solution possible
Thin disk limit, a0
Stress vanishes in outflow
Marginally bound inflow
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BREEZE MODELS
Bound, viscous inflow Unbound, very slow
outflow Viscous stress important in outflow
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WIND MODELS
Bound, viscous inflow Unbound, dynamical
outflow Viscous stress unimportant in outflow
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WIND MODELS
OUTFLOW CAN BE SUBSONIC OR SUPERSONIC BUT
REQUIRES HIGH ENERGY INPUT (?)
SUPERSONIC
SUBSONIC
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CONCLUSIONS

• A new type of ADIOS solution
• well-mixed outflow
• Explains ?R scaling
• Inflow and outflow exchange M, L, but little E
• Energy to drive outflow comes from center
• Total energy supply Eacc?acc??/R
• Fraction ? to outflow, 1-? carried outward by
  inflowing gas
• Details of inner accretion flow determine ?, ?
• Applications SS433, Galactic Center

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Started 1987 AAS, Pasadena Gestation period 4
months

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Started 1998 AAS, San Diego Gestation period 7
months
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Started 1998 Texas Symposium, Paris Gestation
period 5 years
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Started 1999 KITP BH Meeting, Santa Barbara
Gestation period 8 years

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Started 2009 BlandfordFest, Stanford Gestation
period ??

arXiv??10.2327v1 astro-ph.HE 17 Oct 20??