Jet-Disk Connection in AGNs

1
Central Engine of Active Galactic Nuclei 2006
Jet-Disk Connection in AGNs
Jian-Min Wang Key Laboratory for Particle
Astrophysics Institute of High Energy
Physics Chinese Academy of Sciences
2

• 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

3

• High spatial resolution
• dynamics and radiation
• BH mass and spin formation
• BH mass and the Eddington ratios

4
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

5
Blandford Znajek (1977) Citation frequency
24yr-1
Blandford Begelman (1999) Citation frequency
57yr-1
Blandford Payne (1982) Citation frequency
41yr-1
Rawlings Suanders (1991) Citation frequency
20yr-1
Rees et al. (1982) Citation frequency 18yr-1
6
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
7
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

8

• individuals

9
NGC 4261 (Jones et al. 1997)
1 mas 0.2 pc
8.3 GHz image
10
Accretion disk observed by VLBI
Standard disks work in these objects
11
NGC 4151 250pc (Mundell et al. 2003)
NGC 1068 (Gallimore et al. 2004)
12
Radio galaxies M87

• Harms et al. (1994) gaseous disk Junor,
  Biretta Livio (1999)
• Rlt18pc 2109M?

30-100 RS
H?
13
Radio galaxy 3C 120(Marscher et al. 2002)
14
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 10RS, but jets are much wider than this
  region.

15

• Statistic tests

16
Jet-disk connection statistical tests

• Difficulties
• 1) Doppler boosting
• 2) disk luminosity contaminated by jet
• 3) black hole mass and bolometric luminosity

17
Jet kinetic luminosity

• Rawlings Saunders (1991)
• Celotti Fabian (1993)
• Hirotani et al. (2004)

18
Jet-disk connection observational tests

• Rawlings Saunders (1991)
• Sample 39 FR II24 RGs

19

• Questions
• 1) Undergoing processes in radio lobe and the
  central engine are NOT happening simultaneously.
• 2) The covering factors are same in different
  AGNs?

20
Xu, Livio Baum (1999)
409 sources 162 Seyfert galaxies 136 quasars 107
radio galaxies 4 BL Lacs
21
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
22
Jet formation observational tests

• Celotti Fabian (1993)

• Celotti et al. (1997)

Correlation is so faint!
23
Cao Jiang (2001)
Extended radio luminosity and line luminosity
24

• Wang, Luo Ho (2004)

Eddington ratio determines jet-dominance!!!
25
Liu et al. (2006) single line luminosity
26
Jet-disk connection continuum tests
Maraschi Tavecchio (2003) a small sample of 16
blazars BZ process with a rough equipartition
jet power
SED model
27

• 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).

28

• Question what determine the radio loudness?

29
Radio-loudness, BH mass and Eddington ratios

• Laor (2000)

30
Ho (2002)
31
McLure Jarvis (2004) SDSS
The fraction of RL AGN is a function of BH mass
32
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
33

• Comparison with
• X-ray Binaries/Microquasars

34
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)

35
Accretion states and Radio-loudness
Koerding et al. (2006)
Esin et al. (1997)
36
XMMRXTE Miller et al. (astr-oph/0605190)

• SWIFT J1753.5-0127
• Cold comp kT0.2keV
• Hard stateLX/LEdd0.003
• Disk 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!

37
Accretion Mode in BL LacsRLQs(Wang, Ho
Staubert 2002, 03)
HST host-resolved sample
BL Lacs HBLs LBLs
38
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
39
fraction of radio-loud AGNs

• Quasars (Best et al. 2005) 2215 SDSS RLQ
  (0.03ltzlt0.3)

RL Lradgt 1023 WHz-1
40

• 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 Rgt100 (Komossa et al.
  2006), we need to study the disks in detail.
• Q is Begelmans model working?

41
Super-Eddington accretion disk
How about the radio emission from the porous disk?
42
SDSS data(ROSAT,FIRST,NVSS)(Koerding et al.
2006)
Hardness-intensity diagram
NLS1s
43
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.

44

• Thank you for your attention

45
Macorone et al. (2003)based on Merloni et al.
(2003)
RQ AGNs XBR/micro
quasar
LX/LEdd
46
ADIOS behavior also in MHD...
Hawley Balbus 02
47
2-D, adiabatic ?-model ADIOS
Stone, Pringle Begelman 99
48
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) Begelmans model
• is radio different from the two models?

49
The instability of disk inner region?

• Papoliozou-Pringle instability?
• Photon bubble instability

50
Ho (2006)
51
Chemical component of jet two components
Henri Pellettier (1991) theoretical view
Ghisellini et al. (2005) radio knots hardly
moves
52
Kinetic luminosity dissipation
Kinetic dissipation depends on the composition of
the jets. Here Lrad is the intrinsic radiation
53
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)
54
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?

55
Major questions in Jet Physics

• Jet formation from disk
• Jet propagation large-scale jet and its
  terminations
• Jet collimation

56
outline

• Observations old and new
• Theory why?
• Implications
• perspective

57
Super-Eddington jet (Punsley 2006,
astro-ph/0610042) ?
58

• in Seyfert galaxies
• Radio galaxies
• Marscher et al. (2002)
• BL Lac objects
• Radio-loud quasars
• Radio-quiet quasars

59
Radio-loud AGNs

• Fraction of RLAGN versus BH mass
• Fraction of RLAGN versus redshifts