Transcript Kerr Black Holes in Quasars and the Formation of Jets Roger Blandford, KIPAC Stanford with Jonathan McKinney (KIPAC, Maryland) Sasha Tchekhovskoy (Princeton) Nadia Zakamska (JHU)… and Fermi-LAT team 5 vii.

Kerr Black Holes in Quasars and the
Formation of Jets
Roger Blandford,
KIPAC
Stanford
with
Jonathan McKinney (KIPAC, Maryland)
Sasha Tchekhovskoy (Princeton)
Nadia Zakamska (JHU)…
and Fermi-LAT team
5 vii 2013
Potsdam
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M87
Seven billion solar masses
0.01 light yr~10 m
(Doeleman et al.)
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Potsdam
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Cygnus A
Cygnus A
3C 273
Cygnus A
Pictor A
3C31
NGC 326
3C75
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Potsdam
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Sgr A*
3.76 s magnetar?
4 million solar mass hole
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New Radio Telescopes
ALMA
JVLA
SS433
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SUPERLUMINAL EXPANSION
3C 273
G ~ 10 , ~ 3 (FR 1)
S ~ G3
Strong Doppler
Beaming
Intraday
variability Ginzburg
G
30 v 2012
Do we see all the jet?
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SS433 and the W50 nebula
Ginzburg
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Verification of iron line spin measurement from NGC1365
Sgr A*
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The Bigger Picture
• Galaxy Formation, Evolution/Feedback
–
–
–
–
Major vs Minor mergers
Gas vs Stars
AGN vs Starbursts
Jets vs Winds
• Environmental impact
– (Re-)ionization
– Cluster evolution…
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Scale?
Fermi
• Joint NASA-DOE-Italy- France-JapanSweden, Germany… mission
• Launch June 11 2008
–
Cape Canaveral
• Large Area Telescope: 0.02-300 GeV
–
–
–
–
All sky every 3hr
~100 x Compton Gamma Ray Observatory
~3 g-rays per second
105 electron/positrons per second
• Gamma Ray Burst Monitor
– 0.01-30MeV
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832AGN+268Candidates+594Unidentified!
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H.E.S.S.
VERITAS
MAGIC
•
•
•
•
•
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Cerenkov flashes
0.1-30TeV g-rays
Degree resolution
100 sources
Upgrades
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New Windows
on the Universe
•Ultra High Energy Cosmic Rays
•Source energies up to 100 Joule!
•May be seeing black hole sources
•eg Centaurus A
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Auger
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Quasars for the Impatient
~ 20 examples
G~2
Circinus X-1 (G ~ 15?)
Timescales ~ mass?
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Potsdam
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Pulsar Wind Nebulae
Vela-Pavlov-Chandra
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Potsdam
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Black Hole Birth Cries?
• Long Gamma-ray Bursts
– ts~3-100 s E ~ 1051 erg (beaming)
– ~1d -1yr afterglows
– Associated with SN?; BH/Magnetar formation
– Jets, G > 300?
• Short bursts
– ts~ 0.1-3 s
– Coalescing neutron stars??
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3C120
Do variable g-rays
come from
recollimation shocks?
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3C 279: multi-l observation of g-ray flare
• ~30percent optical polarization
=> well-ordered magnetic field
• t~ 20d g-ray variation
=> r~g2ct ~ pc or tdisk?
• Correlated optical variation?
• Ten day lag!
• X-ray, radio uncorrelated
=> different sites
• Rapid polarization swings ~200o
=> rotating magnetic field
in dominant part of source
• PKS 1510+089 -720o!
r ~ 100 or 105 m?
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Potsdam
Abdo, et al, Hayashida et al
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TeV Gamma-ray variation
• M87
– 1 day
• PKS 1222+21
PKS 1222+21 (Aleksik et al)
– 10 min
• MKN 501
– 5 min?
• PKS 2155-304
– 2 min?
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PKS1510+089
(Wardle, Homan et al)
bapp=45
z=0.36
•Rapid swings of jet,
radio position angle
•High polarization
~720o (Marscher)
•Channel vs Source
•TeV variation
(Wagner / HESS)
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Potsdam
•EBL limit
•rmin ; rTeV>rGeV
(B+Levinson)
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3C454.3
Marscher
2x1050erg s-1 isotropic
Breaks due to recombination radiation?
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Potsdam
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MKN 421
•~5min variation
•Inverse Compton?
•outside gammasphere
•G >100?
•cf GRB
Max-Moerbeck et al
•Fermi vs OVRO
•Jet anatomy?
•g-rays before radio
•Jet physiology?
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Tidal Disruption/QPO Events
• RE J1034+396
– P=1hr?
Reis et al
• Sw J1644+57
– P=200s?
Gierlinski et al
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Potsdam
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Last 8 weeks
GRB 130427A
Most powerful, highest energy
G>1000 No ns
PSR J1745-2900
Sgr A* orbit
3 flares
Rapid flares with
L t >> <u> (vt)3
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Astrophysical Black Holes
• Kerr Metric
– Mass m=M8AU=500M8s=2 x 1062 M8 erg
– Angular momentum a < m
– Event Horizon r+=m+(m2+a2)1/2
– Area A=8pmr+=16pm02, increases
– Irreducible mass m0=m[{1+(1+a2/m2)1/2}/2]1/2
– Reducible mass m-m0<0.29m
– Spin W = a / 4m02
– Ergosphere rergo=m+(m2+a2cos2q)1/2
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Potsdam
W
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Three Approaches
• Fluid dynamics +passive field
– Fluid velocity, scalar + ram pressure
• Classical Electromagnetodynamics
– Maxwell stress tensor + Poynting Flux
• Relativistic Magnetohydrodynamics
– All of the above
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Potsdam
Let there be Light
•
•
•
•
Faraday
Maxwell
Initial Condition
Definition
B
   E
t
E
B j
t
 B 0
 E  
2 A  j

=>Maxwell Tensor, Poynting Flux
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
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Force-Free Condition
E  j  B  0  E  B  E  j  0
(  E)E  B  (B    B  E    E)B
j
B2
• Ignore inertia of matter s =UM/UP>>G2, 1

• Electromagnetic
stress acts on
electromagnetic energy density
• Fast and intermediate wave
characteristics,
30 v 2012
Ginzburg
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How to get Blood from a Stone

Rules of thumb:
 F ~ B R2 ; V ~ W F;

I~ V / Z0; P ~ V I
PWN
AGN
GRB
B
100 MT
1 T
1 TT
W
10 Hz
10 Hz
1 kHz
R
10 km
10 Tm
10 km
V
3 PV
300 EV
30 ZV
I
300 TA
3 EA
300 EA
P
100 XW
1 TXW
10 PXW
B M
W
Unipolar Induction
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Potsdam
EM/RMHD power
• Relativistic Force-Free treatment
E  j  B  0  E  B  E  j  0
– No inertia
• Relativistic MHD
– Inertia
j
(  E)E  B  (B    B  E    E)B
B2
• Where do the currents close?

– EM->Heat, bulk kinetic energy
• How are jets powered?
– Disk or hole?
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Force-Free Electrodynamics
in Kerr Spacetime
• F.J=0 div TEM=0
– Pair production necessary
 xf,t
– Conserved F, G
– I(F), V(F), W(F)
• Boundary conditions
– EM finite for infalling observer
• Kerr-Schild or numerical kludge
• Energy flows out at horizon in non-rotating frame
• Energy flows in at horizon in rotating frame
• Circuit analysis
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Telegraphers’ Equations
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On the dragging of inertial frames
• Newtonian:
– Consider a “Uranus” with S.L=0, r=const.
– Let S=(Sr,0,Sf)
– d2S/dt2=-(GM/r3)S
• Kerr metric:
–
–
–
–
Circular, equatorial orbit
S=(-WSf, Sr,0,Sf)
Parallel-propagate along geodesic
d2S/dt2=-(GM/r3)S
• Independent of a including sign!
 wBL=W-r-3/2ut-1=3r-5/2/2-ar-3+…
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Dipolar or Quadrupolar?
Even field
Odd current
Odd field
Even current
W
x
.
Lovelace, Camenzind, Koide, RB
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Potsdam
Also prograde vs retrograde?
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Steady, Radiative Accretion
• Thin disk, slow inflow v, mass per radius 
Torque G, Specific angular momentum l
Angular velocity W, Energy e = -Wl/2
 v

0
 v  const
t
r

v G


0
 v  G  const
t
r
r
e  (WG  ve)
W
de

G
 S  3v
t
r
r
dr
Local energy radiated is
vii 2006
Santa Fe
3 x11the
binding energy released
G
Adiabatic Disks
• Outflows,winds, jets
remove, mass, angular
momentum, energy
• Thick disks
– Ion pressure
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•
•
•
Dissipated energy heats ions
Poor ion-electron coupling
Cold electrons don’t radiate
Radio galaxies
– Radiation pressure
•
•
•
•
Ý 1

Thomson scattering optical depth
Photons trapped within
Advected inwards
BALQs
Ý 1

11 vii 2006
Santa Fe
•
•
•
Relativistic Jets Powered by Black
Hole Spin
Thick disks spin down hole
electromagnetically
Thin disks spin up hole through
accretion
Jet Fuel
10
Ý
M
ÝE
M
1
Width ~WM
Jet properties depend
upon mass supply rate
and history.
0.1
11 vii 2006
Santa Fe
M
Magnetically-choked Accretion Flows
• Robust, collimated jets
– >105 m
• Build up strong dipolar field
– Thick spinning disks, suppress MRI
– Not quadrupolar
• Efficient extraction of spin energy-> jets
– Prograde (not retrograde) more efficient
• Magnetic collimation
– Poorly collimated, slower winds
• QPOs,
– Helical instability (m=1) ~W/4, Q~100 (jet) ~3 (disk)
• Strong intermittency
– Acceleration
5 vii 2013
McKinney, RB;
McKinney, Tschekovskoy, RB
Tschevoskoy et al
Potsdam
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Potsdam
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Magnetically-choked Accretion Flows
• Robust, collimated jets
– >105 m
• Build up strong dipolar field
– Thick spinning disks, suppress MRI
– Not quadrupolar
• Efficient extraction of spin energy-> jets
– Prograde (not retrograde) more efficient
• Magnetic collimation
– Poorly collimated, slower winds
• QPOs,
– Helical instability (m=1) ~W/4, Q~100 (jet) ~3 (disk)
• Strong intermittency
– Acceleration
5 vii 2013
McKinney, RB;
McKinney, Tschekovskoy, RB
Tschevoskoy et al
Potsdam
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Potsdam
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SKA and CTA
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Potsdam
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LIGO, LISA, Nanograv…
RIP
• Merging Black
Holes
– Ultimate test of
dynamical, strong
General Relativity
– Orbit, plunge…
– Background
• Millisecond pulsar
array
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Potsdam
– Fermi + radio (44)
45
– 40 ns timing accuracy
Faraday Rotation
Simulation
Observation
Zavala& Taylor 2005
Broderick & McKinney
Signature of toroidal field/axial current
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Potsdam
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Imaging a Black Hole?
• For M87 and Galactic Center,
– 2m ~10as ~ 0.3 mm/RE
• Event Horizon Telescope (Doeleman et al)
– ALMA VLBI
Dexter, McKinney, Agol
ALMA
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Summary
•
•
•
•
•
•
•
•
Black Holes common in Galaxy, AGN, GRB
Masses and spins can be high
Multi-l observations of large jet samples
Large Lorentz factors inferred.
3D RMHD simulations now very powerful
Kerr holes probably power ultrarelativistic jets
Magnetic->Leptonic->Hadronic transitions
Provide ingredients for extreme acceleration
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