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Jet-Disk Connection in AGNs

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. Jet-disk connection is a fundamental problem in AGN research scale size: disk ~ 0.1pc

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Jet-Disk Connection in AGNs

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  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: feedback

  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 1068 (Gallimore et al. 2004) NGC 4151: 250pc (Mundell et al. 2003)

  12. Radio galaxies: M87 • Harms et al. (1994): gaseous disk; Junor, Biretta & Livio (1999) • R<18pc: 2×109M⊙ 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 II+24 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. Celotti & Fabian (1993) Celotti et al. (1997) Jet formation: observational tests 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. XMM+RXTE: Miller et al. (astr-oph/0605190) • SWIFT J1753.5-0127: Cold comp: kT~0.2keV Hard state:LX/LEdd~0.003 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 Lacs+RLQs(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 (0.03<z<0.3) RL: Lrad> 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 R>100 (Komossa et al. 2006), we need to study the disks in detail. Q: is Begelman’s 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) Begelman’s model is radio different from the two models?

  49. The instability of disk inner region? • Papoliozou-Pringle instability? • Photon bubble instability

  50. Ho (2006)

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