The total power and the age of AGN radio jets

1. The total power and the age of AGN radio jets Hirotaka Ito Waseda University Collaborators Motoki Kino SISSA Nozomu Kawakatu SISSA Naoki Isobe ISAS/JAXA ISS Science Project Office Shoichi YamadaWaseda University @ Relativistic Jets: The Common Physics of AGN, Microquasars and Gamma-Ray Bursts 2005

2. OUTLINE １．Introduction - motivation of present study ２．Cocoon model - brief review of cocoon - construction of analytical model - methods for estimating power and age ３．Results - estimated power and age of 5 FRII radio galaxies ４．Discussions and Conclusions - implications of our results - future works

3. OUTLINE １．Introduction - motivation of present study ２．Cocoon model - brief review of cocoon - construction of analytical model - methods for estimating power and age ３．Results - estimated power and age of 5 FRII radio galaxies ４．Discussions and Conclusions - implications of our results - future works

4. Relativistic jets in radio galaxies Jets from AGN carries huge amount of energy flux ・portion of its energy goes to electrons via shocks ・observed as radio lobes Cygnus A (VLA 1.4 GHz) Recent progress by observations (X-ray, radio) Synchrotron radio Non-thermal electrons + Energies of Inverse Compton X-ray Magnetic fields However, fraction of thermal component and protons are not constrained from observation Prevented from estimating total energy flux

5. ICM reverse shock AGN jet forward bow shock To conquer this we propose a simple model of shock dynamics Powerful radio galaxies forms a shock via interaction with intra-cluster medium (ICM) and forms a cocoon Analytical model describing cocoon expansion (Kino & Kawakatu 2005) comparison Observational data Sketch of AGN jet (FR II) in ICM (credit; CXC) We probe totalkinetic power and source age

6. OUTLINE １．Introduction - motivation of present study ２．Cocoon model - brief review of cocoon - construction of analytical model - methods for estimating power and age ３．Results - estimated power and age of 5 FRII radio galaxies ４．Discussions and Conclusions - implications of our results - future works

7. ICM reverse shock AGN jet forward bow shock jet shocked jet matter Sketch of AGN jet (FR II) in ICM (credit; CXC) A brief review of jet and cocoon dynamics reverse shock contact discontinuity Cocoon natural by-product of a supersonic jet through a denser ambient medium - energy injection forward shock kinetic power of jet (Lj) Includes contribution from “invisible” particles such as protons and/or thermal e+e- shocked ICM Construction of analytical model enables the estimation of Lj

8. vc Ah vh Ac jet cocoon Intra-Cluster Medium Summary of the present work the comparison of observed shape and model (on FR II) Cocoon shape & ICM density Lj & tage Super Nova Sedov-Taylor solution (E, tage) AGN cocoon (FR II) this work (Lj, tage) We don’tknow the absolute value of total kinetic power

9. Basic equations in our model balance between jet thrust and ambient ram pressure assumptions ：eq. of motion （jet axis） Strong shock balance between cocoon pressure and ambient ram pressure ：eq. of motion （lateral） ~ constant kinetic energy of jet converts to internal energy and work ~c energy equation ： ：cross section of j :total power Ac cocoon head cocoon 　　：ambient density ：cross section of ：cocoon length cocoon body ：cocoon width ：velocity of ：lateral velocity cocoon head ：volume of cocoon ：jet velocity

10. Analytic solution approximation density profile： lateral expansion： Solutions are as follows; cocoon evolution in declining ambient density

11. Matching of observation and model sources rh ：cocoon length FRII radio sources with measured ambient density rｃ：cocoon width reference Ah ：cross section of cocoon head cocoon Cygnus A, 3C223, 3C284, 3C263, 3C219 ρa ：ICM density cross sectional are of radio lobe at hot spot ～ pa ：ICM pressure α：density power-law index = 0 observed quantities radio area of radio lobe at hot spot X-ray determination of X： we assume self-similar rc /rh = conditions (I) Contrains Lｊ and tage (II) (III)

12. OUTLINE １．Introduction - motivation of present study ２．Cocoon model - brief review of cocoon - construction of analytical model - methods for estimating power and age ３．Results - estimated power and age of 5 FRII radio galaxies ４．Discussions and Conclusions - implications of our results - future works

13. Cygnus A (3C405) z~0.0565 Lj > LEdd (erg/s) BH mass： Allowed region for Lj and tage minimum mass accretion rate normalized by corresponding Eddington accretion rate 10 100 (Myr)

14. precession? Increasing density? double hot spot not appropriate for our steady jet assumption not appropriate for our model Other Sources 3C223 3C284 z~0.1368 z~0.2394 144kpc 190kpc 3C263 3C219 35kpc z~0.6563 z~0.1744 87kpc

15. OUTLINE １．Introduction - motivation of present study ２．Cocoon model - brief review of cocoon - construction of analytical model - methods for estimating power and age ３．Results - estimated power and age of 5 FRII radio galaxies ４．Discussions and Conclusions - implications of our results - future works

16. Summary By constructing analytical model for cocoon expansion we probe 5 FRII radio galaxies Cygnus A, 3C223, 3C284, 3C263, 3C219 Our main purpose is to constrain total kinetic power of jet estimates of in previous studies based on observations (e.g. Rawlings & Saunders 1991) :total energy of non-thermal electron and equipartition magnetic field :fraction of in total energy free parameter in present study by solving equation of motions is eliminated includes contribution of ‘invisible’ particles

17. e- e- e+ e+ Implications from our results Our cocoon model predicts typically high energy conversion rate Compared with previous studies Is typically one order higher existence of invisible particles are dynamically important Future works 2D HD simulation to check our model (e.g. estimates of ) Anti-matter (e+e-) bubble?? Baryon loading?? unveil the particle contents in the cocoon p