Simulations of AGN jets on 100 kpc scale

Simulations of AGN jets on 100 kpc scale Salvatore Cielo, MPIA Heidelberg, DE Andrea V. Macciò, MPIA Heidelberg, DE Vincenzo Antonuccio-Delogu, INAF, Catania, IT

Why are Jets so mysterious? Jet powers are well constrained, but... 2

Why are Jets so mysterious? Jet powers are well constrained, but...? Several unknowns 2

Why are Jets so mysterious? Jet powers are well constrained, but... Duty cycles link to BH accretion? Several unknowns 2

Why are Jets so mysterious? Jet powers are well constrained, but... Duty cycles link to BH accretion? FRI / FR II intrinsic or environment? Several unknowns 2

Why are Jets so mysterious? Jet powers are well constrained, but... Duty cycles link to BH accretion? FRI / FR II intrinsic or environment? Several unknowns Composition / EoS light/hard: Blandford-Znajek VS Blandford-Payne Blandford, Znajek 1977 2

Why are Jets so mysterious? Jet powers are well constrained, but... Duty cycles link to BH accretion? FRI / FR II intrinsic or environment? Several unknowns Observations: obscured, sparse, small scale gas. Simulations: need to link several physical scales. Composition / EoS light/hard: Blandford-Znajek VS Blandford-Payne Blandford, Znajek 1977 2

So, can jets from AGNs... IN GALAXIES, few Myr...directly reduce SF? (positive VS negative FB) 3

So, can jets from AGNs... IN GALAXIES, few Myr...directly reduce SF? (positive VS negative FB) V. Gaibler (+), 2014 (12),... Silk + 2013, Dubois + 2013,... 3

So, can jets from AGNs... IN GALAXIES, few Myr...directly reduce SF? IN HALOS, >100 Myr...prevent cool flows by heat? (positive VS negative FB) V. Gaibler (+), 2014 (12),... Silk + 2013, Dubois + 2013,... 3

So, can jets from AGNs... IN GALAXIES, few Myr...directly reduce SF? (positive VS negative FB) V. Gaibler (+), 2014 (12),... Silk + 2013, Dubois + 2013,... IN HALOS, >100 Myr...prevent cool flows by heat? Perseus cluster ~150 kpc CHANDRA nasa.gov Complex heating mechanisms (bubbles, etc.) invoked with little testing 3

My setup, in the FLASH code Dark Matter NFW potential (static, spherical, external) Hot halo Isothermal, self-grav + DM hydrostatic equilibrium, rad. cooling (e.g. Mhalo = 2e12 Msun => T ~ 5e6 K) 4

My setup, in the FLASH code Dark Matter NFW potential (static, spherical, external) Hot halo Isothermal, self-grav + DM hydrostatic equilibrium, rad. cooling FRII: recollimation shocks (e.g. Mhalo = 2e12 Msun => T ~ 5e6 K) Jet density contrast 1:100 Pjet = ρjet A vjet 3 = 1e42-1e46 erg/s FRI/FRII: Mach 5 - Mach 100 on/off cycles: 1-100 Myr Box: 60-640kpc Resolution:10-150 pc 4

My setup, in the FLASH code Dark Matter NFW potential (static, spherical, external) Hot halo Isothermal, self-grav + DM hydrostatic equilibrium, rad. cooling FRII: recollimation shocks (e.g. Mhalo = 2e12 Msun => T ~ 5e6 K) Jet density contrast 1:100 Pjet = ρjet A vjet 3 = 1e42-1e46 erg/s FRI/FRII: Mach 5 - Mach 100 on/off cycles: 1-100 Myr Warm gas clouds (1e4 K) in a central galaxy + SF with sink particles. One day. Box: 60-640kpc Resolution:10-150 pc 4

10 42 erg/s 120 kpc Results: Evolutionary stages 5

10 42 erg/s 120 kpc 1. Cocoon and HS formation Results: Evolutionary stages 5

10 42 erg/s 120 kpc 1. Cocoon and HS formation 2. Forward propagation Results: Evolutionary stages 5

10 42 erg/s 120 kpc 1. Cocoon and HS formation 2. Forward propagation 3. Lobes inflation Results: Evolutionary stages 5

10 42 erg/s 120 kpc 1. Cocoon and HS formation 2. Forward propagation 3. Lobes inflation 4. Bubbles (jet off) Results: Evolutionary stages 5

Bubbles still there after.6 Gyr 6

Results: Energy and Volume Coverage p dv Mechanical Work as fraction of Pjet Coupling: (W pdv / t age ) / P jet 1 0.8 0.6 0.4 0.2 1E45 erg/s 1E44 erg/s 1E43 erg/s 1E42 erg/s All gas Lobes/Bubbles only 0 10 0 10 2 t age / Myr Cielo +, in prep. 7

Results: Energy and Volume Coverage p dv Mechanical Work as fraction of Pjet Volume coverage within rcool ~30kpc (2e12 MSun) Coupling: (W pdv / t age ) / P jet 1 0.8 0.6 0.4 0.2 1E45 erg/s 1E44 erg/s 1E43 erg/s 1E42 erg/s All gas Lobes/Bubbles only V C 30 kpc / Vsphere 30 kpc 1 0.8 0.6 0.4 0.2 1E45 erg/s 1E44 erg/s 1E43 erg/s 1E42 erg/s Low res 0 10 0 10 2 t age / Myr Cielo +, in prep. 0 10 1 10 2 t / Myr age 7

Results: Energy and Volume Coverage p dv Mechanical Work as fraction of Pjet Volume coverage within rcool ~30kpc (2e12 MSun) Coupling: (W pdv / t age ) / P jet 1 0.8 0.6 0.4 0.2 1E45 erg/s 1E44 erg/s 1E43 erg/s 1E42 erg/s All gas Lobes/Bubbles only V C 30 kpc / Vsphere 30 kpc 1 0.8 0.6 0.4 0.2 1E45 erg/s Low res 1E44 erg/s 1E43 erg/s 1E42 erg/s FRII can make it... FRI not large enough! 0 10 0 10 2 t age / Myr Cielo +, in prep. 0 10 1 10 2 t / Myr age 7

Results: angle flip 10 45 erg/s ~150 kpc Can the volume fraction increase with multiple injections? 8

Results: angle flip 10 45 erg/s ~150 kpc Can the volume fraction increase with multiple injections? Not really... :( 8

Summary Can we simulate AGNs radio mode with AMR? self-consistently? Do jets have enough energy? Do they affect enough volume in the ISM? 9