Simulations of AGN jets on 100 kpc scale

Transcription

1 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

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

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

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

5 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

6 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

7 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

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

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

10 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 , Dubois ,... 3

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

12 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

13 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: Myr Box: kpc Resolution: pc 4

14 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: Myr Warm gas clouds (1e4 K) in a central galaxy + SF with sink particles. One day. Box: kpc Resolution: pc 4

15 10 42 erg/s 120 kpc Results: Evolutionary stages 5

16 10 42 erg/s 120 kpc 1. Cocoon and HS formation Results: Evolutionary stages 5

17 10 42 erg/s 120 kpc 1. Cocoon and HS formation 2. Forward propagation Results: Evolutionary stages 5

18 10 42 erg/s 120 kpc 1. Cocoon and HS formation 2. Forward propagation 3. Lobes inflation Results: Evolutionary stages 5

19 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

20 Bubbles still there after.6 Gyr 6

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

22 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 E45 erg/s 1E44 erg/s 1E43 erg/s 1E42 erg/s All gas Lobes/Bubbles only V C 30 kpc / Vsphere 30 kpc E45 erg/s 1E44 erg/s 1E43 erg/s 1E42 erg/s Low res t age / Myr Cielo +, in prep t / Myr age 7

23 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 E45 erg/s 1E44 erg/s 1E43 erg/s 1E42 erg/s All gas Lobes/Bubbles only V C 30 kpc / Vsphere 30 kpc E45 erg/s Low res 1E44 erg/s 1E43 erg/s 1E42 erg/s FRII can make it... FRI not large enough! t age / Myr Cielo +, in prep t / Myr age 7

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

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

26 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