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

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

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

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

5. We probe total kinetic power and source age 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 (Kino & Kawakatu 2005) Observational data comparison ICM AGN jet revers e shock forward bow shock Analytical model describing cocoon expansion Sketch of AGN jet (FR II) in ICM ( credit; CXC)

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

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

8. Summary of the present work L j & t age Cocoon shape & ICM density jet cocoon AcAc vcvc vhvh Intra-Cluster Medium AhAh the comparison of observed shape and model (on FR II) We don ’ t know the absolute value of total kinetic power Super Nova Sedov-Taylor solution (E, t age ) AGN cocoon (FR II) this work (L j, t age )

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

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

11. area of radio lobe at hot spot observed quantities r h ： cocoon length r ｃ ： cocoon width A h ： cross section of cocoon head ρ a ： ICM density p a ： ICM pressure α ： density power-law index radio X-ray determination of X ： r c /r h = = 0 we assume self-similar cocoon (I) (III) cross sectional are of radio lobe at hot spot ～ Matching of observation and model (II) conditions Contrains L ｊ and t age FRII radio sources with measured ambient density Cygnus A, 3C223, 3C284, 3C263, 3C219 sources reference

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

13. BH mass ： minimum mass accretion rate normalized by corresponding Eddington accretion rate Cygnus A (3C405) z~0.0565 L j > L Edd Allowed region for L j and t age (erg/s) (Myr) 10100

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

15. OUTLINE １． Introduction ２． Cocoon model ３． Results ４． Discussions and Conclusions - motivation of present study - brief review of cocoon - construction of analytical model - methods for estimating power and age - estimated power and age of 5 FRII radio galaxies - 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 estimates of in previous studies based on observations (e.g. Rawlings & Saunders 1991) Our main purpose is to constrain total kinetic power of jet :total energy of non-thermal electron and equipartition magnetic field :fraction of in total energy free parameter in present study is eliminatedby solving equation of motions includes contribution of ‘invisible’ particles

17. Our cocoon model predicts typically high energy conversion rate Implications from our results 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 Anti-matter (e+e-) bubble?? Baryon loading?? p e+e+ e-e- e-e- e+e+ unveil the particle contents in the cocoon (e.g. estimates of )