Jet-Disk Connection in AGNs

Central Engine of Active Galactic Nuclei 2006

Jian-Min WangKey Laboratory for Particle Astrophysics

Institute of High Energy Physics

Chinese Academy of Sciences

• Jet-disk connection is a fundamental problem in AGN research

scale size: disk ~ 0.1pc jet ~ 10-3pc-10kpc (from inner to lobe)

the powerful jets indicate a deep gravity potential of the supermassive black holes with an accretion disk.

jet likely links with release of disk angular momentum

• High spatial resolution:

dynamics and radiation

• BH mass and spin: formation

BH mass and the Eddington ratios

References• Theory: Blandford & Payne (1982); Rees et al. (1982); Blandford & Znajek (1977); Henri & Pelletier (1991); Ghosh & Abramowicz (1997); Xu & Chen (1997) Blandford & Begelman (1999); Livio et al. (1999); Meier et al. (2002) Balbus & Hawley (2003); Meier (2002); Merloni & Fabian (2002); Livio et al. (2003); Tavecho & Maraschi (2002); Maraschi & Tavecho(2003) Kato et al. (2004); McKinney & Narayan (2006)

• Observations: individual and large sample Rawlings & Suanders (1991); Rawlings & Suanders (1992) Falcke & Biermann (1995); Celotti et al. (1997); Xu et al. (1999) Cao & Jiang (1999); Gu, et al. (2000); Laor (2001) Blandford & Begelman (1999); Wang, et al. (2002,03,04); Mundell et al. (2003) Punsley (2005); Jester (2005); Woo & Urry (2005); Liu et al. (2006); Koerding et al. (2006); Sikora et al. (2006); Greene & Ho (2006); Komossa et al. (2006); Whalen et al. (2006)

• Implications: feedback

Blandford & Znajek (1977)

Citation frequency: 24yr-1

Blandford & Payne (1982)

Citation frequency: 41yr-1

Rawlings & Suanders (1991)

Citation frequency: 20yr-1Rees et al. (1982)

Citation frequency: 18yr-1

Blandford & Begelman (1999):

Citation frequency: 57yr-1

Major questions

• jet formation/ejection from disk: are they really connected? how to form and quench? how to accelerate jet? jet fraction of the energy output from BH accretion?

• jet formation is BH mass-scale free?

• jet component?• jet interaction with surrounding photons from disk, BLR?

All these questions are related with the status of the accretion disk

methodologies

• Individual: monitoring and mapping• Statistic studies: 1) jet indicators: non-thermal emission and high energy emission radio/kinetic luminosity 2) disk indictors: thermal emission BBB, NLR/BLR luminosity• Analogy: compared with X-ray binaries or microquasars

• Numerical simulations

individuals

NGC 4261 (Jones et al. 1997)

8.3 GHz image

1 mas = 0.2 pc

Accretion disk observed by VLBI

Standard disks work in these objects

NGC 4151: 250pc (Mundell et al. 2003)

NGC 1068 (Gallimore et al. 2004)

Radio galaxies: M87• Harms et al. (1994): gaseous disk; Junor, Biretta & Livio (1999)

• R<18pc: 2×109M⊙

H30-100 RS

Radio galaxy: 3C 120(Marscher et al. 2002)

Questions?

• Why ejection is only related with X-ray luminosity variation?

monitoring AGNs show that there is no time lag among the light curves in different bands (Peterson 2004), confronting with the standard disk model (e.g. Clave et al. 1988).

• What kinds of disk model working in AGNs? most of the gravitational energy is dissipated around 10R

S, but jets are much wider than this region.

Statistic tests

Jet-disk connection: statistical tests

Difficulties:

1) Doppler boosting:

2) disk luminosity: contaminated by jet

3) black hole mass and bolometric luminosity

)cos-(1

1

;)()( 30

10

0

II

Jet kinetic luminosity

• Rawlings & Saunders (1991)

• Celotti & Fabian (1993)

• Hirotani et al. (2004)

))(1( 22ee

2BLRKin cmcmncRL

Jet-disk connection: observational tests

• Rawlings & Saunders (1991)• Sample: 39 FR II+24 RGs

kin

jet

luminosity kinetic

luminsity radiation

Q

L

mediumon done workingefficiency :

age lobe : energy; lobe total:

kin

TE

T

EQ

0.20.9NLRkin

LQ

luminosity kinetic

luminosityradiation

kin

rad

Q

L

• Questions:

1) Undergoing processes in radio lobe and the central engine are NOT happening simultaneously.

2) The covering factors are same in different AGNs?

Xu, Livio & Baum (1999)

409 sources:

162 Seyfert galaxies

136 quasars

107 radio galaxies

4 BL Lacs

)quiet-radio( 6.50.45log

)loud-radio( 7.3log61.0)core( log

III] [O

III] [OGHz5 L

LL

Best et al. (2005): SDSS RL AGNs

Radio is independent of

[O III] luminosity!!!!

Are they really different in physical mechanisms?

Rawling & Saunders (1991) line

Jet formation: observational tests

Celotti & Fabian (1993) Celotti et al. (1997)Correlation is so faint!

Cao & Jiang (2001)

Extended radio luminosity and line luminosity

• Wang, Luo & Ho (2004)

Eddington ratio determines jet-dominance!!!

Liu et al. (2006): single line luminosity

Jet-disk connection: continuum tests

Maraschi & Tavecchio (2003): a small sample of 16 blazars

BZ process with a rough equipartition: jet power

SED model

64/1 ;22BZ gMcgaP

• It implies simply that BZ power is independent to the Eddington ratio, however this is supported.

BH is fast spin if BZ works; MCG 6-30-15 is radio faint

• Poloidal magnetic field is needed to produce jet

(Livio, Pringle & King 2003).

R

H

L

L

B

B

acc

jet

2disk

2p ~

• Question: what determine the radio loudness?

Radio-loudness, BH mass and Eddington ratios

• Laor (2000)

Ho (2002)

McLure & Jarvis (2004): SDSS

The fraction of RL AGN is a function of BH mass

Sikora et al. (2006)

Filled circle: BLRGs; open circles: RLQs; cross: open triangles: Seyferts, FR I & FR I; filled stars: PG quasars

The radio-loudness strongly correlates with the Eddington ratios

Comparison with

X-ray Binaries/Microquasars

Jet and states of accretion disk

• Timescale is much longer than that in X-ray binaries and microquasars.

• Fraction of RL AGNs: transition

• Actually we do not know whether there is an evolutionary transition between

RL RQ AGNs (to keep in mind)

Accretion states and Radio-loudness

Koerding et al. (2006)

Esin et al. (1997)

XMM+RXTE: Miller et al. (astr-oph/0605190)

• SWIFT J1753.5-0127: Cold comp: kT~0.2keV

Hard state:LX/LEdd~0.003Disk is still full at low state ！a prominent accretion disk in the low-hard state of the black hole candidate:

Truncated disk?

There are always OUTLIERS!

Accretion Mode in BL Lacs+RLQs(Wang, Ho & Staubert 2002, 03)

BL Lacs: HBLs & LBLs

HST host-resolved sample:

Ghisellini & Celotti (2001)

Ledlow-Owen Plane is divided into two parts:

Cao & Rawlings (2004):

PZ is not powerful enough, but PB is not powerful enough in FR I

fraction of radio-loud AGNs

1. Quasars (Best et al. 2005): 2215 SDSS RLQ (0.03<z<0.3)

1.6BHMf RL: Lrad> 1023 WHz-1

Narrow line Seyfert 1 galaxies

Geene & Ho (2006): 0 - 6% (19 NLS1s) Komossa et al. (2006): 7%(11/128 NL quasars

from Veron-Veron sample)

At high state of AGNs: radio is very faint, only 2.5% RL NLS1 have R>100 (Komossa et al. 2006), we need to study the disks in detail.

Q: is Begelman’s model working?

Super-Eddington accretion disk:

5/45/1

1.01001.040~

: luminosity Max.

apart disk blowing without possible

disk porousbubblesPhoton

m

L

L

LL

E

E

How about the radio emission from the porous disk?

SDSS data+(ROSAT,FIRST,NVSS)(Koerding et al. 2006)

9.354.0log

3

:diagram luminosityfraction disk

BD

keV105.0PL

PLD

PL

ML

LL

LL

L

Hardness-intensity diagram

NLS1s

Summary

• We understand the jet-disk connection insufficiently and still have many problems

• jet formation, what parameters depends on?

• What is origin of radio emission in RQ-AGNs?

• Do microquasars/X-ray binaries correspond to all kinds of AGNs? How to correspond?

• Are there two modes of super-Eddington accretion? for some exceptionals.

Thank you for your attention

Macorone et al. (2003)based on Merloni et al.

(2003)

RQ AGNs

XBR/micro quasar

LX/LEdd

Hawley & Balbus 02

ADIOS behavior also in MHD...

Stone, Pringle & Begelman 99

2-D, adiabatic -model: ADIOS

inM

outM

outinacc MMM

Questions?

• Miller et al. (2006) find that there is filled disk in low state of Swift objects.

• The truncated disk model may be wrong?

• For very high states (super-Eddington accretion):

1) classical slim disk (Abramowicz et al. 1988)

2) Begelman’s model

is radio different from the two models?

The instability of disk inner region?

• Papoliozou-Pringle instability?• Photon bubble instability

Ho (2006)

Chemical component of jet: two components

Henri & Pellettier (1991): theoretical view Ghisellini et al. (2005): radio knots hardly moves

Kinetic luminosity: dissipation

Kinetic dissipation depends on the composition of the jets.

Here Lrad is the intrinsic radiation

Jet component: pair + p-e- plasama

• Mrk 421 (Celotti et al 1997): ADAF model

However ADAF is NOT

able to produce pairs

(Kusunose et al. 1995) ,

the ADAF model

should be modified!

Ghisellini et al. (2005)

Open questions

• What are differences in RL-AGNs and RQ-AGNs?• What is origination of radio emission in RQ-AGNs?• Do microquasars/X-ray binary correspond to all kinds of

AGNs? How to correspond?• Are there two modes of super-Eddington accretion?

Major questions in Jet Physics

• Jet formation from disk

• Jet propagation: large-scale jet and its terminations

• Jet collimation

outline

• Observations: old and new

• Theory: why?

• Implications

• perspective

Super-Eddington jet (Punsley 2006, ast

ro-ph/0610042) ?

• in Seyfert galaxies

• Radio galaxies

Marscher et al. (2002)

• BL Lac objects

• Radio-loud quasars

• Radio-quiet quasars

Radio-loud AGNs

• Fraction of RLAGN versus BH mass

• Fraction of RLAGN versus redshifts