AGN Outflows in Dynamic ICMs: Winds and Twists
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1 AGN Outflows in Dynamic ICMs: Winds and Twists Tom Jones University of Minnesota Pete Mendygral (UMN, Cray Computer) David Porter (UMN) Klaus Dolag (MPA, U Munich) 11/29/2012 Binary Black Holes & Dual AGN 1
2 Outline AGN outflows (radio jets) are major dynamical & thermodynamical ICM components AGN/ICM interactions may provide insights to AGN & ICM physics Is binarity in radio mode AGNs useful as a tool in these investigations? 11/29/2012 Binary Black Holes & Dual AGN 2
3 Dave DeYoung was keenly interested in AGN/ICM interactions (from 2007 Anchorage Workshop) 3D Buoyant Bubble AGN-made ICM cavity: Role of the ICM magnetic field g hydro t = 75 Myr β 0 = 3000 t = 75 Myr β 0 = 120 t = 150 Myr Bubble mass fraction r 0 = 2 kpc x 0 = 15 kpc ρ bub /ρ icm = x34x34 kpc x=0.13 kpc DeYoung, O Neill & Jones May, 2007 Extragalactic Jets 3
4 Radio AGNs are Common in Clusters Cluster cores Perseus Cluster outskirts A kpc Xray w/ radio contours Croston + X-ray (red) & radio (green) Rudnick + 11/29/2012 Binary Black Holes & Dual AGN 4
5 Importance: Energy Input to ICM Can Be Large Rafferty + 11/29/2012 Binary Black Holes & Dual AGN 5
6 Importance: Dynamics Reflect ICM Motions/Structure NGC kpc O Dea & Owen λ21cm U gal ~ 2000 km/s τ AGN > 2x10 8 yr 3C 84 ~540 kpc Sijbring & debruyn λ49cm 11/29/2012 Binary Black Holes & Dual AGN 6
7 Some Known to be Binary (Many Might Be) Binary Example: 3C 75 A400 NGC 1128 ~ 8kpc separation Red (visible) Blue (radio) 11/29/2012 Binary Black Holes & Dual AGN 7
8 Binary Example: AS345 ~ 40 kpc separation Grey (visible) Contours (radio) 11/29/2012 Binary Black Holes & Dual AGN 8
9 Binary Example: FIRST J Visible + radio contours radio ~15 kpc separation 11/29/2012 Binary Black Holes & Dual AGN 9
10 Given the commonality of AGNs in ICMs The Challenge: Decipher complex morphological (& other) clues to establish useful dynamical diagnostics: E.G., ICM flow properties ICM magnetic field properties Jet physical properties Define key Jet/ICM interaction parameters We ve mostly explored through simulations 11/29/2012 Binary Black Holes & Dual AGN 10
11 Previous Generation Jet Simulations in Static ICMs (3D MHD) e.g., O Neill, Mendygral & Jones 2009 Bipolar, collimated Mach 30 (internal) jet outflows L jet = 1.2x10 46 erg/s (combined jets at full power) Steady or intermittent (50%, 26 Myr cycle) r jet = 3 kpc ρ jet /ρ 0 = 0.01 Toroidal jet B field at source (β = P g /P M ~ 100; B j ~ 10 µg) Passive `CR electrons, shock injection & DSA Adiabatic & radiative (synch, IC) losses AGN at center of ~ 4x10 14 M o cluster (NFW potential) Static ICM, kt ICM ~3keV (~ Perseus) Double β profile with random density fluctuations Tangled ICM magnetic field <β plasma >~ 100 (range ~ 30:1000) (<B core > ~ 7µG) No radiative cooling of ICM 11/29/2012 Binary Black Holes & Dual AGN 11
12 Illustration: Intermittent Jets Magnetic Field Intensity Blue (AGN plasma) Red (ICM plasma) t = 170 Myr 11/29/2012 Binary Black Holes & Dual AGN 12
13 Synthetically Observed & Actual Energetics Comparisons Good to ~ 50% 11/29/2012 Binary Black Holes & Dual AGN 13
14 On the Other Hand: Real ICMs are Dynamic: Bullet Cluster 1E Chandra + HST 11/29/2012 Binary Black Holes & Dual AGN 14
15 Two Classes of More Realistic Simulations: AGN Jets in simple, but dynamic media AGN Jets in self-consistent ICMs 11/29/2012 Binary Black Holes & Dual AGN 15
16 Example: Bipolar AGN Jets in a Turbulent ICM Wind: Narrow Angle Tail (NAT) FRI Source (Porter ) Code: MHD TVD with passive CR electrons (CGMV) Box: 1 Mpc x 1 Mpc x 200 kpc 2000x2000x400 =1.6x10 9 zones x = 0.5 kpc Jet Power: 5x10 44 erg/s Jet Radius: 5 kpc Bending Radius: ~ 20 kpc (M j /M ICM ~ 2) Simulation Duration: 215 Myr Tail Length: ~ 600 kpc 11/29/2012 Binary Black Holes & Dual AGN 16
17 Emergent Jets: NAT Simulation Setup: U jet = 0.044c R jet = 5 kpc ρ jet = 0.1 <ρ icm > M jet = u jet /s jet = 3 β jet = P mag /P gas ~ 10 (toroidal field) ICM: θ u jet z y x Bending Radius: R b /R j ~(M j /M w ) 2 (P j /P i ) for (P j /P i ) = 1 U icm = 2000 km/s θ = 30 degrees M w = u icm /s icm = 1.5 P icm =P jet =1.8x10-11 dy/cm 2 <n icm >=.001 cm -3 B rms = 2.2 µg <β icm > = 100 Turbulent ICM: Outer scale 20 kpc Kolmogorov u icm Jet-Wind Plane R b /R j ~ (M j /M i ) 2 = 4 So R b ~ 20 kpc 11/29/2012 Binary Black Holes & Dual AGN 17
18 Kinetic Energy Deposition KE in ICM Rest Frame Jet-wind plane 11/29/2012 Binary Black Holes & Dual AGN 18
19 Vorticity (Shear, turbulence) Volume Rendered t = 215 Myr 11/29/2012 Binary Black Holes & Dual AGN 19
20 Magnetic Field Injection/Amplification Volume Rendered t = 215 Myr 11/29/2012 Binary Black Holes & Dual AGN 20
21 Synthetic Synchrotron Emission (Using included Cre population) 178 MHz 215 Myr 11/29/2012 Binary Black Holes & Dual AGN 21
22 Self-Consistent ICM Example: Intermittent Bipolar AGN Jets in a Nominally Relaxed ICM Extracted from Cosmological Simulation (SPH MHD): Wide Angle Tail (WAT) FR II Source Mendrygral Code: MHD TVD (grid-based) with passive CR electrons (CGMV) Box: 1 Mpc 3 ; zones x = 1 kpc Jet Power: 6x10 44 erg/s Jet Radius: 3 kpc Jet Velocity: v j = 10 4 km/s Jet Density: ρ j = 4x10-28 g/cm 3 Toroidal Magnetic Field (β = 1, 10, 100) Cluster (7 Gyr since major merger): Mass = 1.5 x M o ; kt ~ 1.5 kev; c s ~ 650 km/s B core ~ 5 µ G 11/29/2012 Binary Black Holes & Dual AGN 22
23 Overview of Selected Cluster z = 0 1 Mpc 11/29/2012 Binary Black Holes & Dual AGN 23
24 Cluster Magnetic Field 11/29/2012 Binary Black Holes & Dual AGN 24
25 Initial ICM Gas Entropy Slices with Velocity Vectors Cross winds up to 450 km/sec Bar shows jet axis 11/29/2012 Binary Black Holes & Dual AGN 25
26 Evolution of AGN Cavity Note distortions From axial symmetry ( Launch cylinder visible) 11/29/2012 Binary Black Holes & Dual AGN 26
27 Synthetic X-Ray Image (divided by β-law) 11/29/2012 Binary Black Holes & Dual AGN 27
28 Synthetic Radio Images 11/29/2012 Binary Black Holes & Dual AGN 28
29 Back to Binary AGNs: 3C 75 A400 Merging clusters v ~ km/s Merging galaxies v ~ 400 km/s Projected separation ~ 7 kpc Blue (X-ray) Pink (radio) 11/29/2012 Binary Black Holes & Dual AGN 29
30 Model 3C 75 as Pair of Orbiting BHs in Cross Wind Yokosawa & Inoue v w = 1100 km/s (almost in plane) Orbital diameter 8kpc Orbital period 110 Myr 11/29/2012 Binary Black Holes & Dual AGN 30
31 General idea of Expected Behavior (Yokosawa + Ballistic Model) 11/29/2012 Binary Black Holes & Dual AGN 31
32 Yokosawa + Ballistic Model V j 2000 km/s 11/29/2012 Binary Black Holes & Dual AGN 32
33 Our MHD Simulation Set Up: Box: 500 kpc X 250 kpc X 500 kpc (1084 X 542 X 1084) grid x = 0.5 kpc ICM: ρ ICM = 5 x g/cm 3 P ICM = 1.3x10-11 dyne/cm 2 v x = 1100 km/s (v y = v z = 0) v x /c s = M ICM = 1.67 Turbulent ICM: <v turb > RMS = 150 km/s, <B turb > RMS = 2 µg outer scale 30 kpc Jets: (paired & orthogonal to AGN orbit) r j = 3 kpc v j = 1.5x10 4 km/s P j = P ICM = 1.3x10-11 dyne/cm 2 ρ j = 5 x g/cm 3 v j /c sj = M j = 7.2 β = P g /P M = 10 L j = 5 x erg/s orbital diameter = 12 kpc (x-y plane) orbital period = 91 Myr 11/29/2012 Binary Black Holes & Dual AGN 33
34 Crude Comparison Simulation: Jet mass fraction 3C 75: radio in pink t= 215 Myr Roughly similar scales 11/29/2012 Binary Black Holes & Dual AGN 34
35 t = 215 Myr (~ 2 binary orbits) Jet mass fraction color Jet break : z l b ~ (M j /M ICM ) 2 r j x Varies during Orbit (v w + v o ) < l b > ~ 60 kpc Tail lengths ~ 300 kpc 11/29/2012 Binary Black Holes & Dual AGN 35
36 Evolution of Mass Fraction 11/29/2012 Binary Black Holes & Dual AGN 36
37 Thanks! 11/29/2012 Binary Black Holes & Dual AGN 37
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