5 iv 2012 CIFAR 1

(How) Do Spinning Holes make Jets?

Roger Blandford,KIPAC

Stanfordwith

Jonathan McKinney (KIPAC, Maryland)Sasha Tschekovskoy (Princeton)

Nadia Zakamska (JHU)

Sackler Lecture Princeton22 iv 2010

Cygnus A

3C31

3C75

Extragalactic Jets

Pictor A

M87

NGC 326

5 iv 2012 CIFAR

Pictor A

Current FlowNonthermal emission is ohmic dissipation of current flow?

Electromagnetic Transport1018 not 1017 ADC not ACNo internal shocksNew particle acceleration mechanisms

Pinch stabilized by velocity gradient?

Equipartition in core

Wilson et al

3

5 iv 2012 CIFAR 4832AGN+268Candidates+594Unidentified!

3C454.3

5 iv 2012 CIFAR 5

2x1050erg s-1 isotropicBreaks due to recombination radiation?

Marscher

Radio Monitoring (OVRO 40m)

• ~1500 sources• Radio and g-ray active• Spectrum, polarization

5 iv 2012 CIFAR 6

Max-Moerbeck etal

Rapid MAGIC variation

• PKS 1222+21– 10 min

• MKN 501– 2min?

• PKS 2155-304– “Few hr”?

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PKS 1222+21 (Aleksik et al)

How typical?How fast is GeV variation?

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? => common emission site

• X-ray, radio uncorrelated => different sites

• Rapid polarization swings ~200o => rotating magnetic field in dominant part of source

Abdo, et al Nature, 463, 919 (2010)

r ~ 100 or 105 m?

5 iv 2012 8CIFAR

PKS1510+089

(Wardle, Homan et al)

5 iv 2012 CIFAR 9

z=0.36• Rapid swings of

jet, radio position angle• High polarization ~720o (Marscher)

• Channel vs Source• TeV variation (Wagner / HESS)

• EBL limit• rmin ; rTeV>rGeV

(B+Levinson)

bapp=45

Jansky VLA (New Mexico)

5 iv 2012 CIFAR 10

27 antennae, 1-50GHz (+0.08GHz)10xsensitivity… 50 mas resolution

SS433 and the W50 nebula

Chandler Outflows, Winds, and Jets Workshop, March 2012

11

ALMA First results

5 iv 2012 CIFAR 12

Atacama desert 5km high66 telescopes, 300m- 1cm eventually ~ 5mas resolution

CIFAR 135 iv 2012

B

M

Rules of thumb:

~ F B R2 ; V ~ W F; I~ V / Z

0; P ~ V I

PWN AGN GRB

B 100 MT 1 T 1 TT

/2 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

Unipolar Induction

UHECR!

€

m =m0

1 − β2; β = Ωm < 2−1/ 2

5 iv 2012 CIFAR

Intermediate Mass Supply

• Thin, cold, steady, slow, radiative disk

• Specific energy e = -Wl/2

€

G − ′ M l = const ≈ 0

dL

dr=

d(ΩG − ′ M e)

dr≈ 3 ′ M

de

drG

Energy radiated is 3 x the local energy loss14

5 iv 2012 CIFAR

Low, High Mass Supply

• M’<<M’E, tenuous flow cannot heat electrons and cannot cool

• M’>>M’E, dense flow traps photons and cannot cool • Thick, hot, steady, slow, adiabatic disk• Bernoulli function: b =e+h

€

G − ′ M l ≈ 0

ΩG − ′ M b ≈ 0

⇒ b ≈ −2e > 0

G

Energy transported by torque unbinds gas => outflow

ADiabatic Inflow-Outflow Solution15

5 iv 2012 CIFAR 16

W

x

.

Dipolar or Quadrupolar?

Even field Odd current

Lovelace, Camenzind, Koide, RB

x x x

Odd field Even current

Also prograde vs retrograde?

5 iv 2012 CIFAR 17

CIFAR 18

“Observing” Simulated Jets

Synchrotron Radiation

€

IνΩ(ν , to) = dzδ 2 j'ν 'Ω'∫ (ν /δ, to)e− dzδ −1κ '(ν /δ ,to )∫

δ =1

γ(1−Vz)

Sν (ν , to) =1

ad2dxdyI∫

νΩ(ν , to)

5 iv 2012

• We know P’, B’, N’, V on grid• Work in jet frame• Rotate spatial grid so that observer along z direction• Shear in t – z space introducing to=t-z

• Make emission model• eg j’ ~ P’ B’3/2 ’n -1/2; ’~ k P’B’2 ’n -3

• Polarization – perpendicular to projected field in cm frame

t

z

to

z’

z

Vß

“Observing” Simulated Jets

Inverse Compton Radiation• Work in jet frame

• Compute incident radiation along all rays from earlier observer times

• Compute j nW directly

5 iv 2012 CIFAR 19

Observer

sq

r

[r-s,to-s(1-cosq)]

z

“Observing” Simulated Jets

Pair Opacity

5 iv 2012 CIFAR 20

€

κ = dsdΩdνNνΩ (r r −

r s ∫ , to − s(1− cosφ),ν )σ PP (1− cosφ)

• External and internal radiation• Internal radiation varies

5 iv 2012 CIFAR 21

Disk

Light

Optical emission from jet with g ~ 3-4

Zakamska, RB & McKinney in prep

Quivering Jets• Observe g-rays (and optical in

3C279)• Gammasphere tgg~1, 100-1000m ~

Eg• Rapid variation associated with

convected flow of features (2min in Mkn 501)

• Slow variation associated with change of jet direction on time scale determined by dynamics of disk (precession?) or limited by inertia of surrounding medium or both as with m=1 wave mode.

5 iv 2012 CIFAR 22

5 iv 2012 CIFAR 23

Total Flux and Degree of Polarization

Summary

5 iv 2012 CIFAR 24

• New observations of AGN and stellar relativistic jets• Fermi, MAGIC, optical polarimetry, JVLA, ALMA…• 3D Black Hole MHD simulations possible for >106 m• Efficient energy extraction• Powerful winds• Jet Disk Oscillations• “Observe” simulated relativistic jets• Radio, g-rays, optical polarization

Dynamical elements • Bulk flow• Shocks• Shear flow • Plasmoids, flares, minijets,magnetic

rockets…– Lorentz boosting

• Precession– Disk– m=1 instability

• Turbulence

5 iv 2012 CIFAR 25

Each of these elements changes the field and the particles

Pair vs Ion Plasmas

• Pairs must be heavily magnetized to avoid radiative drag

• Circular polarization, Faraday rotation/pulsation

• Expect? pairs, field todecrease, ions to increase along jet

5 iv 2012 CIFAR 26

CIFAR 275 iv 2012

Particle acceleration in high s environments

• Internal shocks are ineffectual• Reconnection can be efficient

– E>B??• Shear flow in jets

– Full potential difference available particles accelerated when undergo polarization drift along E

– UHECR (eg Ostrowski & Stawarz, 2002)

• Fast/intermediate wave spectrum– Nonlinear wave acceleration(Blandford 1973…)

• Mutual evolution of wave cascade and particle distribution function– Charge starvation (eg Thompson & Blaes 1997)

• Force-free allows E>B - catastrophic breakdown

Particle Acceleration

5 iv 2012 CIFAR 28

• S-C-1 transition quite high in BLLacs• “Theoretically” Eg<a-1 mec2~60MeV• cf Crab Nebula, UHECR• Large scale electric fields• Lossy coax??• Follow particle orbits.• Which particles carry the current• Is the momentum elctromagnetic?

5 iv 2012 CIFAR 29

Faraday Rotation

Broderick & McKinney

Signature of toroidal field/axial current

Rotation from sheath

Observations ???

Simulation

5 iv 2012 CIFAR 30

Telegraphers’ Equations

5 iv 2012 CIFAR 31

Relativistic Reconnection

McKinney & Uzdensky

• High s flow• Hall effects may save Petschek mechanism• Anomalous resistivity?• Also for AGN

Petschek

GRBs?

5 iv 2012 CIFAR 32

Inhomogeneous Sources • Radio synchrotron

photosphere, r ~ l– Doppler boosting

• Compton gammasphere, r ~ E?– Internal, external radiation– Test with variability, correlation

• Electron acceleration – >100 TeV electrons

5 iv 2012 CIFAR 33

S

n E

S C-1

Summary• Protostars->GRBs->Quasars• Location, mechanism, collimation,

origin…? • FGST+TeV+multi-l observations of blazars• Major monitoring campaigns• Rotating polarization, rapid variation• GRMHD simulations answering basic

questions about flows, dynamics• “Observations” of simulations now

possible to (in)validate simple phenomenological models and test against data and “best” examples. 5 iv 2012 CIFAR 34

CIFAR 35

3D GRMHD Simulations• >105m Kerr-Schild, HARM, 512x768x64

– Quasi-steady state

• Build up flux –back reaction– Thick spinning disks, suppress MRI– Dipolar (not quadrupolar) makes jets

• Efficient extraction of spin energy-> jets– Prograde (not retrograde) more efficient

• Wind outflows– Poorly collimated, slow

• QPOs, – ~70m, a~ 0.9; Q~100 (jet) ~3 (disk)

• Strong intermittency– Helical instability m=1

5 iv 2012

McKinney, RB; McKinney, Tschekovskoy, RB

Tschevoskoy et alTalk on MONDAY