how to form ultrarelativistic jets speaker: jonathan c. mckinney, stanford oct 10, 2007 chandra...
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![Page 1: How to Form Ultrarelativistic Jets Speaker: Jonathan C. McKinney, Stanford Oct 10, 2007 Chandra Symposium 2007](https://reader036.vdocuments.net/reader036/viewer/2022062516/56649d535503460f94a2f328/html5/thumbnails/1.jpg)
How to Form Ultrarelativistic Jets
Speaker: Jonathan C. McKinney, Stanford
Oct 10, 2007
Chandra Symposium 2007
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M87 Jet Formation/Interaction
Junor (1999) & Biretta (1999,2002)
X-ray: NASA/CXC/CfA/W.Forman et al.; Optical: DSS
NASA/CXC/H.Feng et al.
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Black Hole Accretion Systems
Mirabel & Rodriguez (Sky & Telescope, 2002)
1038erg/s
M~10M¯
1044erg/s
M~107M¯
1052erg/s
M~3M¯
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BH Accretion/Wind/Jet Issues
– Origin of organized field
– Poynting jet / disk wind / neutrino power
– Disk-wind-jet coupling
– Jet collimation, acceleration, stability
– Mass-loading and angular structure (GRB light curves)
– Reconnection paradigm vs. shocks
– AGN feedback
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Blandford & Znajek
Disk
Poloidal FieldAssumptions:•Kerr BH (slowly rotating)
•Force-free ED or EM>MA
•Axisymmetric
•Stationary
Solve:•Maxwell’s Equations
OR
•Conservation equations
Find:•Outward Flux of Energy
•Magnetic Field Structure
(monopole or parabolic)
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Energy Extraction• Dimensional Argument
• BZ Solution for (split) monopole field
BZ Efficiency factor:
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BZ vs. McKinney
(McKinney 2006a)
(McK
inney &
Nara
yan
20
06
b)
Next: 3D, Stability, Cold GRMHD (add mass, keep T=0)
•Blandford’s swindle
•Collimation: disk currents beat hoop-stresses
•Realistic disk field?
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GRMHD
Poloidal Field
Disk
Assumptions:•Kerr BH (a/M~0.94~spin eq.)
•Kerr-Schild coordinates
•Matter + fields (MA+EM)
•Ideal MHD, ideal (=4/3) gas
•Axisymmetric, nonradiative
•Initial hydro-eq.thick torus (H/R» 0.2)
Solve:•Time-dependent conservation equations
•Induction equation with r¢B=0 constraint Gammie, McKinney, Toth (2003)
McKinney & Gammie (2004)
Gammie, Shapiro, McKinney (2004)
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Accretion Disk Structure
•Ordered at poles
•Random in equator
Log of mass density Poloidal Field
McKinney & Gammie (2004)
Poy
ntin
g Je
t“M
atte
r” J
et
CORONA: MA~EM
FUNNEL: EM dominated
JETS: Unbound, outbound flow
Flow Structure
•Evacuated at poles
•Turbulent in equator
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Blandford-Payne DiskField Geometry
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Common Field Lines
123
4
5
6
7
8
9
Final
State
Time
Avg.
State
Common
Temporary
Never
Balbus & Hawley (MRI) [1]Gammie & Krolik [2,3]Effect of reconnections [4,5]Lovelace or Blandford-Payne [6,7]Konigl & Vlahakis [6,7,~9]Uzdensky, Matsumoto [8]Blandford & Znajek [9]
McK
inney (2
005)
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Disk-Jet Coupling
• Nearly stationary force-free jet with BP-like scaling• MRI drives disk+corona to support funnel field• No Blandford-Payne field from disk
McK
inney &
Nara
yan (2
00
6a)
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Large Scale Jet
McKinney (2006c)
Magnetic Domain:
r<~1000M
Thermal Domain: r>~1000M
r»104 GM/c2
1010cm
t»104 GM/c3
0.1s
Adiabatic expansion of shocked material
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Density and Field: Large scales
McKinney (2006c)
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Picture
Mag Jet
Shock
Z
on
e
Kinetic or Thermal Jet
Coronal Outflow/JetCoronal Wind
r» 102-103M
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Summary of Science Learned
• Jets driven by BH are clean and so fast
• Winds driven by disk are dirty and slow
• Jet collimated by corona/wind– not by internal rotation (i.e. hoop stresses)
• Kink instability probably not effective
• Reconnection not necessary for dissipation of magnetic energy