1. 1 Radio-mode Feedback Alex Wagner Geoff Bicknell (with previous contributions by Ralph Sutherland & Curtis Saxton)

2. Research School of Astronomy & Astrophysics 2 Aims Provide “sub-grid” physics for cosmological AGN feedback calculations Understand the early stages of evolution of radio galaxies Theoretical basis for GMT and SKA observational programs

3. Research School of Astronomy & Astrophysics 3 [OIII] and radio morphology of MRC0406- 244 [OIII] morphology [OIII] velocity Contours of line-free continuum [OIII] velocity dispersion Nesvadba et al. ’08)

4. Research School of Astronomy & Astrophysics 4 Effect of an inhomogeneous medium

5. Research School of Astronomy & Astrophysics 5 Typical run (D’)

6. Research School of Astronomy & Astrophysics 6 Velocity-power diagram

7. Research School of Astronomy & Astrophysics 7 Filling factor and cloud size Low filling factor R cloud,max =50 pc R cloud,max =10 pc

8. Research School of Astronomy & Astrophysics 8 3D view of Run 3D’ Blue-green jet plasma Purple clouds Forward shock of energy- driven bubble

9. Research School of Astronomy & Astrophysics 9 Comparison of R-t relation with analytic energy-driven bubble Analytic solution approached as filling factor decreases

10. Research School of Astronomy & Astrophysics 10 Energy imparted to clouds Substantial fraction of jet energy ends up in warm clouds

11. Research School of Astronomy & Astrophysics 11 Effect of filling factor Initial decrease of filling factor increases volume of flood channels for jet plasma Increased cloud ablation

12. Research School of Astronomy & Astrophysics 12 Effect of cloud size Clouds generated using Fourier code (Ralph) with a minimum wave number k min Maximum cloud radius R cloud,max = 1/(2 k min ) Unsurprisingly larger clouds are harder to accelerate

13. Research School of Astronomy & Astrophysics 13 Mechanical advantage

14. Research School of Astronomy & Astrophysics 14 Summary of cloud velocity vs Jet power

15. Research School of Astronomy & Astrophysics 15 Comparison with observations Lehnert et al. (2011) 691 radio galaxies (Different estimates of P jet from 1.4 GHz radio power)

16. Research School of Astronomy & Astrophysics 16 Distribution of velocities Most of the galaxies with outflows have v > velocity dispersion

17. Research School of Astronomy & Astrophysics 17 3D jet plasma visualization - Ajay Limaye (NCI)

18. Research School of Astronomy & Astrophysics 18 3D density visualization