theoretical calculations of the inner disk’s luminosity scott c. noble, julian h. krolik (jhu)...
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![Page 1: Theoretical Calculations of the Inner Disk’s Luminosity Scott C. Noble, Julian H. Krolik (JHU) (John F. Hawley, Charles F. Gammie) 37 th COSPAR 2008, E17](https://reader035.vdocument.in/reader035/viewer/2022070412/56649d555503460f94a32167/html5/thumbnails/1.jpg)
Theoretical Calculations of the Inner Disk’s LuminosityScott C. Noble, Julian H. Krolik (JHU)
(John F. Hawley, Charles F. Gammie)
37th COSPAR 2008, E17July 16th, 2008
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Steady-State Model: Novikov & Thorne (1973)
GR model of radiatively efficient disks
F(r,a) T(r,a) and Rin
Observations MBH, aBH
F
Wr
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Steady-State Model: Novikov & Thorne (1973)
Assumptions:
1) Stationary gravity
2) Equatorial Keplerian Flow
Thin, cold disks
o Tilted disks?
3) Time-independent
4) Prompt, local dissipation of
stress to heat
5) Conservation of M, E, L
6) Zero Stress at ISCO
o Magnetic fields?
o Need dynamic simulations!
F
Wr
For steady-state model context:Shafee, Narayan, McClintock (2008)
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Previous Work
• De Villiers, Hawley, Hirose, Krolik (2003-2006)
MRI develops from weak initial field.
Significant field within ISCO up to the horizon
• Beckwith, Hawley, Krolik (2008)
– Rad. Flux ~ Stress
– Uncontrolled loss of dissipated energy
Krolik, Hawley, Hirose (2005)
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Our Method: Simulations
• HARM: Gammie, McKinney, Toth (2003)
• Axisymmetric (2D)
• Total energy conserving
• Modern Shock Capturing techniques (greater accuracy)
• Improvements:– 3D
– More accurate (higher effective resolution)
– Stable low density flows
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Our Method: Simulations• Improvements:
– 3D– More accurate (higher
effective resolution)– Stable low density flows
– Cooling function:
• Control energy loss rate
• Parameterized by H/R
• tcool ~ torb
• Only cool when T > Ttarget
• Passive radiation
• Radiative flux is stored for self-
consistent post-simulation
radiative transfer calculation
H/R ~ 0.1 aBH = 0.9
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Our Method: Radiative Transfer
• Full GR radiative transfer – GR geodesic integration
– Doppler shifts
– Gravitational redshift
– Relativistic beaming
– Uses simulation’s fluid vel.
– Inclination angle survey
– Time domain survey
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Disk Thermodynamics
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Disk Thickness
dVH
HARM3D
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Departure from Keplerian Motion
HARM3D
dVH
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Magnetic Stress
dVH
HARM3D
NT
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Fluid Frame Flux
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Observer Frame Luminosity: Angle/Time Average
HARM3D
NT
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Observer Frame Luminosity: Angle/Time Average
NT
HARM3D
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Assume NT profile for r > 12M .
Observer Frame Luminosity: Angle/Time Average
NT
HARM3D
L = 4% L
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Observer Frame Luminosity: Angle/Time Average
NT
HARM3D
L = 9% L
Assume NT profile for r > 12M .
Assume no differenceat large radius.
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Summary & Conclusions
• We now have the tools to self-consistently measure dL/dr from GRMHD
disks
• 3D Conservative GRMHD simulations
• GR Radiative Transfer
• Luminosity from within ISCO diminished by
• Photon capture by the black hole
• Gravitational redshift
• tcool < tinflow
Possibly greater difference for aBH < 0.9 when ISCO is further out
of the potential well.
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Future Work
• Explore parameter space:
• More spins
• More H/R ‘s
• More H(R) ‘s
• Time variability analysis
•Impossible with steady-state models
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EXTRA SLIDES
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Accretion Rate
1000
Steady State Period = 7000 – 15000M
Steady State Region = Horizon – 12M
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Observer Frame Luminosity: Time Average
NT
HARM
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Previous Work
• De Villiers, Hawley, Hirose, Krolik (2003-2006)
MRI develops from weak initial field.
Significant field within ISCO up to the horizon.
Hirose, Krolik, De Villiers, Hawley (2004)