How do Black Holes Get Their Gas? - TAPIR at Caltechphopkins/talks/joelfest_2010.pdf · How do...
Transcript of How do Black Holes Get Their Gas? - TAPIR at Caltechphopkins/talks/joelfest_2010.pdf · How do...
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How do Black Holes Get Their Gas?
Eliot Quataert, Lars Hernquist, T. J. Cox, Kevin Bundy, Jackson DeBuhr,Volker Springel, Dusan Keres, Gordon Richards, Josh Younger,
Desika Narayanan, Paul Martini, Adam Lidz, Tiziana Di Matteo, Yuexing Li, Alison Coil, Adam Myers, Patrik Jonsson, Chris Hayward
Philip Hopkins
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• Focus: Most luminous QSOs (~1-10 Msun/yr)
• ‘Bottleneck’ at <10-50pc: BH begins to dominate the potential (e.g. Goodman et al., Jogee et al., Martini et al.)
~5 kpc
500 pc
<10 pc
<0.1 pc Viscous disk/MRI
“bars within bars”
BH/nuclei merging
?gravitational instability? (NO...?)clumps? (NO)viscosity? (NO)MHD wind? (NO)
galaxy-galaxy mergers
disk instabilities
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• If BHs trace spheroids, then *most* mass added in violent events that also build bulges
• Galaxy merger: good way to get lots of gas to small scales!
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• If BHs trace spheroids, then *most* mass added in violent events that also build bulges
• Galaxy merger: good way to get lots of gas to small scales!
• Problem: Scale of merger: ~100 kpc Viscous disk: ~0.1 pc
• Solution 1: simple prescription• Solution 2: re-simulate (“zoom in”) and see what happens!
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Simulations:
FOLLOWING THE GAS IN...
• Here: Focus on robust conclusions
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Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Here: Focus on robust conclusions
Tuesday, December 25, 12
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Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Gas+Stars
• Here: Focus on robust conclusions
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Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Gas+Stars
• Self-gravity!
• Here: Focus on robust conclusions
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Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Gas+Stars
• Self-gravity!
• Cooling
• Here: Focus on robust conclusions
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Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Gas+Stars
• Self-gravity!
• Cooling
• Star formation
• Here: Focus on robust conclusions
Tuesday, December 25, 12
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Krumholz & Tan
Hicks et al.
Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Gas+Stars
• Self-gravity!
• Cooling
• Star formation
• Here: Focus on robust conclusions
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Krumholz & Tan
Hicks et al.
Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Gas+Stars
• Self-gravity!
• Cooling
• Star formation • ‘Feedback’ - Admit we don’t understand it!
• Here: Focus on robust conclusions
Tuesday, December 25, 12
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Krumholz & Tan
Hicks et al.
Simulations:
FOLLOWING THE GAS IN...
• Need to include:
• Gas+Stars
• Self-gravity!
• Cooling
• Star formation • ‘Feedback’ - Admit we don’t understand it!
• Here: Focus on robust conclusions
masers (Greenhill, Kondratko)
starbursts(Downes+Solomon, Scoville, et al.)
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Tidal torques ⇒ large, rapid gas inflows (e.g. Barnes & Hernquist 1991)Tuesday, December 25, 12
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Triggers Starbursts (e.g. Mihos & Hernquist 1996)Tuesday, December 25, 12
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Fuels Rapid BH Growth? (e.g. Di Matteo et al., PFH et al. 2005)
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Large-scale simulation: follow gas to sub-kpc scales
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Now: Re-simulate central kpc at high-res Follow gas to ~10 pc
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Continue, re-simulate central regions, down to 0.1pc resolution
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How do massive BHs get their gas?
CAN WE FUEL THE MONSTER?
• Cascade of instabilities: merger not efficient inside ~kpc
• Any mechanism that gets to similar densities at these scales will do the same
• Instabilities change form at BH radius of influence
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Sub-kpc scales: “Stuff within Stuff”
• Diverse morphologies on sub-kpc scales: not just bars!
• Inflow is not smooth/continuous
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Sub-kpc scales: “Stuff within Stuff”
• Diverse morphologies on sub-kpc scales: not just bars!
• Inflow is not smooth/continuous
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Weakly bar-unstable disk (less inflow)
• Key parameter: Gas driven in, vs. pre-existing bulge/BH mass
Gas-rich merger (lots of inflow)
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Weakly bar-unstable disk (less inflow)
• Key parameter: Gas driven in, vs. pre-existing bulge/BH mass
Gas-rich merger (lots of inflow)
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• Stars torquing on gas
gas (contours)
stars (color)
• Gravity dominates torques from 0.1 - 10,000 pc:
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• Build analytic models:• Structure• Growth rates• Stability• Inflow rates
gas (contours)
stars (color)
How does this work?
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• Build analytic models:• Structure• Growth rates• Stability• Inflow rates
gas (contours)
stars (color)
How does this work?
standard (dissipationless) formulation: spiral waves carry the angular momentum: (Lynden-Bell & Kalnajs ‘72)
Minflow = �[k, |a|]/� R2 � |a|2
|kR|2Mdisk
Mtot
Mgas
tdyn(|kR|� 1)
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• Build analytic models:• Structure• Growth rates• Stability• Inflow rates
gas (contours)
stars (color)
How does this work?
standard (dissipationless) formulation: spiral waves carry the angular momentum: (Lynden-Bell & Kalnajs ‘72)
Minflow = �[k, |a|]/� R2 � |a|2
|kR|2Mdisk
Mtot
Mgas
tdyn(|kR|� 1)
with shocks & dissipation:
� |a| Mgas
tdyn >100x larger!!!
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kpc
10 pc
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kpc
10 pc
Actual inflow rate
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kpc
10 pc
Actual inflow rate
Prediction (gravitational torques with shocks)
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kpc
10 pc
Actual inflow rate
Prediction (gravitational torques with shocks)
No dissipation (Lynden-Bell+ ‘71)
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Can we build a better accretion rate estimator?
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Can we build a better accretion rate estimator?
Derive ‘Gravitational Torque’ Rate:
M � 10 M� yr�1� Disk
Total
�5/2M�1/6
BH, 8 Mgas, 9 R�3/20,100
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Act
ual i
nflow
rate
ont
o BH
[Msu
n/yr]
from 100 pc
from 1 kpc
� c2s �gas ��1Viscous: � G2 M2
BH � c�3sBondi:
Inflow from ~kpc to ~0.1 pc is NOT viscous or Bondi-Hoyle:
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Act
ual i
nflow
rate
ont
o BH
[Msu
n/yr]
from 10 pc
from 100 pc
Gravitational Prediction
from 1 kpc
from 50 pc
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Act
ual i
nflow
rate
ont
o BH
[Msu
n/yr]
from 10 pc
from 100 pc
Gravitational Prediction
from 1 kpc
from 50 pc
True
Inflo
w R
ate
[Msu
n/yr]
Predicted (New Gravitational Scaling)Tuesday, December 25, 12
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So, what about the “small” scales near the BH?
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~10 pc scales: Nuclear eccentric disks
• Inside BH radius of influence: develop thick, precessing disks
• Need both star formation and self-gravity
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epicycle
Keplerian potentials are special:
� = �Hence, closed elliptical orbits!
Eccentric/lopsided disks (m=1 modes) are special in a near-Keplerian potential
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epicycle
Keplerian potentials are special:
� = �Hence, closed elliptical orbits!
Eccentric/lopsided disks (m=1 modes) are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
�� � cos m�
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epicycle
Keplerian potentials are special:
� = �Hence, closed elliptical orbits!
Eccentric/lopsided disks (m=1 modes) are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
�� � cos m�
Generically, force some deviations/torques/etc:
����v
Vc
��� ����
�
� Mdisk(< r)MBH
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epicycle
Keplerian potentials are special:
� = �Hence, closed elliptical orbits!
Eccentric/lopsided disks (m=1 modes) are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
�� � cos m�
Generically, force some deviations/torques/etc:
����v
Vc
��� ����
�
� Mdisk(< r)MBH
But, if (and only if) m=1:����v
Vc
��� ����
�
�
Tuesday, December 25, 12
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Relic, ~pc-scale nuclear stellar disk....
• Gas-stellar exchange dramatically enhances torques
• Drives ~10 Msun/yr inflow
• Leave relic stellar disks?
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• These are observed! M31, NGC4486B, many candidates (NGC 404,507,1374,3706,4073,4291,4382,5055,5576,7619, VCC128, M32,83)
M31:
Lauer et al. 1993Kormendy & Bender 1999
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• These are observed! M31, NGC4486B, many candidates (NGC 404,507,1374,3706,4073,4291,4382,5055,5576,7619, VCC128, M32,83)
M31:
Lauer et al. 1993Kormendy & Bender 1999
• M31 disk has ~0.1-1 MBH in old stellar mass• Outer radius R~1-10 pc• Moderate thickness, high eccentricity
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M31
• These are observed! M31, NGC4486B, many candidates (NGC 404,507,1374,3706,4073,4291,4382,5055,5576,7619, VCC128, M32,83)
• “run backwards”: the M31 disk implies accretion at ~0.5-3 Msun/yr (~LEdd) for ~100 Myr (~ MBH) !
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What about the obscuration from these disks?
• Lots of gas in this disk during the inflow stages...
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What about the obscuration from these disks?
• Lots of gas in this disk during the inflow stages...
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What about the obscuration from these disks?
• The eccentric disk IS the torus!
• Lots of gas in this disk during the inflow stages...
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What about the obscuration from these disks?
cs~20 km/s cs~50 km/scs~30 km/s
cs~5 km/s cs~10 km/s cs~15 km/s
• The eccentric disk IS the torus• Occurs even if allow cooling and no stellar feedback!
• Heating by bending/warping modes, themselves excited by the eccentric pattern
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SummaryØ Fueling Most Luminous BHs:
Global gravitational instabilities CAN power ~10 Msun/yr! Really!• New Mdot estimator: neither viscous nor Bondi
Ø “Stuff within Stuff”: Cascade of instabilities with diverse morphology• Doesn’t matter how first ‘get down’ from large scales
Ø Accretion rates & orientations are stochastic • Vary on all timescales• Angular momentum changes rapidly - no correlation with host disk
Ø The torus is the disk: a dynamical accretion driver • Bending/warping instabilities: thick even without stellar feedback
Ø Stellar nuclear disk ‘relics’: M31 & 4486b: Can we directly observe the ‘fossil’ of the accretion driver & torus ?
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• Observed surface densities and kinematics arise naturally
Masers (Kondratko, Greenhill, et al.)AO (Hicks, Davies, et al.)
5 pc
Obscuration and the ‘torus’
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• Compare column density distributions: edge-on
gas has NO substructure
observed(Risaliti, Treister, Malizia)
quasi-virial clumps
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• Gravity dominates torques from 0.1 - 10,000 pc
Torq
ues a
t R
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• m=1 ‘slow’ modes are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
number of ‘arms’
�� � cos m�
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• m=1 ‘slow’ modes are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
number of ‘arms’
�� � cos m�
|e| � 1�
Response: � = �2 �m�2
Tuesday, December 25, 12
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• m=1 ‘slow’ modes are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
number of ‘arms’
�� � cos m�
|e| � 1�
Response: � = �2 �m�2
Near a BH:1�� 1
(1�m)�2
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• m=1 ‘slow’ modes are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
number of ‘arms’
�� � cos m�
|e| � 1�
Response: � = �2 �m�2
Near a BH:1�� 1
(1�m)�2
m �= 1 :
�2 � r�3 :1�� 0
|e| ��
���
�Mdisk(< r)
MBH
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• m=1 ‘slow’ modes are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
number of ‘arms’
�� � cos m�
|e| � 1�
Response: � = �2 �m�2
Near a BH:1�� 1
(1�m)�2
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• m=1 ‘slow’ modes are special in a near-Keplerian potential
Disturb the stars with some perturbation in the disk:
number of ‘arms’
�� � cos m�
|e| � 1�
Response: � = �2 �m�2
Near a BH:1�� 1
(1�m)�2
m = 1 :�� 0 (resonance)
|e| � ���
• Strong torques can propagate to all r (even << 0.1pc) INDEPENDENT of Mdisk(<r)/MBH
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Large-Scale Tides are Not Important for AGN:
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The Effective Stellar Feedback on Small Scales:(REQUIRE SOME SUB-RESOLUTION MODEL)
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A “No Feedback” ISM is Ruled Out on Small Scales:
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But qualitative conclusions are insensitive to the gas microphysics
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Vertical Torus Structure
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Vertical Torus Structure
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Mis-alignments with the parent disk are common
• Implications for:• BH spin• BH-BH mergers• Recoils• Variability
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Torus-Host disk misalignments:
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