How to Form Ultrarelativistic Jets Speaker: Jonathan C. McKinney, Stanford Oct 10, 2007 Chandra Symposium 2007.

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Presentation transcript:

How to Form Ultrarelativistic Jets Speaker: Jonathan C. McKinney, Stanford Oct 10, 2007 Chandra Symposium 2007

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.

Black Hole Accretion Systems Mirabel & Rodriguez (Sky & Telescope, 2002) erg/s M~10M ¯ erg/s M~10 7 M ¯ erg/s M~3M ¯

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

Blandford & Znajek Disk Poloidal Field Assumptions: 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)

Energy Extraction Dimensional Argument BZ Solution for (split) monopole field BZ Efficiency factor:

BZ vs. McKinney (McKinney 2006a) (McKinney & Narayan 2006b) Next: 3D, Stability, Cold GRMHD (add mass, keep T=0) Blandford’s swindle Collimation: disk currents beat hoop- stresses Realistic disk field?

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)

Accretion Disk Structure Ordered at poles Random in equator Log of mass density Poloidal Field McKinney & Gammie (2004) Poynting Jet “Matter” Jet CORONA : MA~EM FUNNEL : EM dominated JETS : Unbound, outbound flow Flow Structure Evacuated at poles Turbulent in equator

Blandford-Payne Disk Field Geometry

Common Field Lines 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] McKinney (2005)

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 McKinney & Narayan (2006a)

Large Scale Jet McKinney (2006c) Magnetic Domain: r<~1000M Thermal Domain: r>~1000M r»10 4 GM/c cm t»10 4 GM/c 3 0.1s Adiabatic expansion of shocked material

Density and Field: Large scales McKinney (2006c)

Picture Mag Jet Shock Zone Kinetic or Thermal Jet Coronal Outflow/Jet Coronal Wind r» M

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