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 )