1 / 18

Radio-mode Feedback

Radio-mode Feedback. Alex Wagner Geoff Bicknell (with previous contributions by Ralph Sutherland & Curtis Saxton). Aims. Provide “sub-grid” physics for cosmological AGN feedback calculations Understand the early stages of evolution of radio galaxies

agalia
Download Presentation

Radio-mode Feedback

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

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

  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. [OIII] and radio morphology of MRC0406-244 Nesvadba et al. ’08) [OIII] morphology Contours of line-free continuum [OIII] velocity [OIII] velocity dispersion

  4. Effect of an inhomogeneous medium

  5. Typical run (D’)

  6. Velocity-power diagram

  7. Filling factor and cloud size Low filling factor Rcloud,max=50 pc Rcloud,max=10 pc

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

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

  10. Energy imparted to clouds Substantial fraction of jet energy ends up in warm clouds

  11. Effect of filling factor Initial decrease of filling factor increases volume of flood channels for jet plasma Increased cloud ablation

  12. Effect of cloud size Clouds generated using Fourier code (Ralph) with a minimum wave number kmin Maximum cloud radius Rcloud,max = 1/(2 kmin) Unsurprisingly larger clouds are harder to accelerate

  13. Mechanical advantage

  14. Summary of cloud velocity vs Jet power

  15. Comparison with observations Lehnert et al. (2011) 691 radio galaxies (Different estimates of Pjet from 1.4 GHz radio power)

  16. Distribution of velocities Most of the galaxies with outflows have v > velocity dispersion

  17. 3D jet plasma visualization - Ajay Limaye (NCI)

  18. 3D density visualization

More Related