Hirotaka Ito Waseda University 　　　 Collaborators

Motoki Kino 　 　 SISSA 　 　　

　　　　　　　　　Naoki Isobe 　 ISAS/JAXA ISS Science Project OfficeISAS/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 The total power and the age age of of

AGN radio jetsAGN radio jets

OUTLINE１． 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

OUTLINE１． 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

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

We probe total kinetic power and source age

To conquer this we propose a simple model of shock dynamicsPowerful radio galaxies forms a shock via interaction with

intra-cluster medium (ICM) and forms a cocoon

(Kino & Kawakatu 2005)

Observational data

comparison

ICM

AGN jetreverse

shockforward

bow shock

Analytical model describing cocoon expansion

Sketch of AGN jet (FR II) in ICM (credit; CXC)

OUTLINE１． 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

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

Cocoonnatural 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 jetreverse

shockforward bow

shock

- energy injection

kinetic power of jet (Lj)

Construction of analytical model enables the estimation of Lj

Summary of the present work

Lj & tage

Cocoon shape

&ICM density

jet

cocoon

A c

v c

v h

Intra-Cluster

Medium

Ah

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, tage)

AGN cocoon (FR II) 　 this work 　 (Lj, tage)

coco

onA c

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

ac PP balance between cocoon pressure and ambient ram pressure

energy equation

~c

~ constant

Analytic solution

Solutions are as follows;

approximation

density profile ： lateral expansion ：

X

agecc t

tAtA

)(

cocoon evolution in declining ambient density

area of radio lobe at hot spot

observed quantities

rh ： cocoon length

r ｃ ： cocoon width

Ah ： cross section of cocoon head 　　　　　

ρa ： ICM density

pa ： ICM pressure

α ： density power-law index

radio

X-ray

determination of X ： rc /rh =

= 0

we assume self-similar

coco

on

(I)

(III)

cross sectional are of radio lobe at hot spot～

Matching of observation and model

(II)

conditions

X

agecc t

tAtA

)(

Contrains L ｊ and tage

FRII radio sources with measured ambient density

Cygnus A, 3C223, 3C284, 3C263, 3C219

sources

reference

OUTLINE１． Introduction

２． Cocoon model

３． Results４． 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

solM9105.2 BH mass ： 147103 ergsLedd

minimum mass accretion rate normalized by corresponding

Eddington accretion rate

Cygnus A (3C405) z~0.0565

Lj > LEdd

Allowed region for Lj and tage

MyrtMyr age 4318

146145 102.5106.9 ergsLergs j

(erg

/s)

4510

(Myr)

kpcrh 60~ 2150~ kpcAh

16.003.0~ Edd

j

L

L4610

4710

4810

10 100

Other Sources

14

4k

pc

87k

pc

35kpc

190kpc

3C223

3C219 3C263

3C284

precession?double

hot spotnot appropriate for our steady jet assumption

Increasing density?

not appropriate for our model

kpcrh 380~

24000~ kpcAh

kpcrh 260~24000~ kpcAh

kpcrh 240~

21500~ kpcAh

kpcrh 405~23900~ kpcAh

z~0.6563

z~0.2394

z~0.1744

z~0.1368

OUTLINE１． 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

SummaryBy 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 eliminated by solving equation of motions

includes contribution of ‘invisible’ particles

Our cocoon model predicts typically

high energy conversion rate

Implications from our results

EddjEdd LLL ~1.0~

Compared with previous studiesIs typically one order higher

existence of invisible particles are dynamically important

Future works2D HD simulation to check our model

Anti-matter (e+e-) bubble??Baryon loading??

p

e+ e-e-

e+unveil the particle contents in the cocoon

(e.g. estimates of )