1. 1 Astrophysical Jets Mario Livio Space Telescope Science Institute

2. 2 Which Systems Have Highly Collimated Jets ? ObjectPhysical System Young Stellar ObjectsAccreting Star HMXBsAccreting NS X-ray TransientsAccreting BH LMXBsAccreting NS Supersoft X-ray SourcesAccreting WD Symbiotic starsAccreting WD Pulsars (?)Rotating NS Planetary Nebulae Accreting Nucleus or Interacting Winds Stellar ObjectPhysical System AGNAccreting Supermassive BH GRBsAccreting BH Extragalactic

3. 3 Disks around Young Stars STScI-PRC99-05b

4. 4 M87: AGN from 200,000 light years to 0.2 light year

5. 5 Superluminal Motion in M87 HST-1 Do FR I radio galaxies have relativistic jets like BL Lacs?

6. 6 “Superluminal” sources GRS 1915+105 V ~ 0.9c Extragalactic jets show V > 0.995c

7. 7 Gamma Ray Bursts Fruchter et al. 2006

8. 8 STScI-PRC99-32 Southern Crab Nebula He2-104 Symbiotics

9. 9 Planetary Nebulae STScI-PRC97-38b

10. 10 Point-Symmetric Planetary Nebulae IC 4634

11. 11 Point-Symmetric Planetary Nebulae

12. 12 Point-Symmetric Planetary Nebulae

13. 13 Vermeulen et al. 1993 SS 433

14. 14 Supersoft X-Ray Source RXJ 0513-69 Southwell et al. 1996

15. 15 Recurrent Novae and Symbiotics U Sco (1999) Lépine, Shara, Livio & Zurek 1999 Hillwig, Livio & Honeycutt 2004

16. 16 Pulsar Jets Chandra Crab PulsarVela Pulsar Chandra

17. 17 Do Jets Require an Accretion Disk? What are the absolutely necessary ingredients for the mechanism of jet acceleration and collimation? Have disk? YSOsYes (but maybe funnels?) PNeYes (but maybe funnels?) SSSYes H/LMXBsYes BHXTsYes GRBsWe don’t know AGNYes (?) (but maybe ion torus and surrounding gas pressure? Fabian & Rees 1995)

18. 18 [OI] 6300 Profiles for T Tauri Stars Redshifted component not seen because of disk. Edwards et al. 1987 Livio & Xu 1997

19. 19 X-Ray Spectroscopy of Accretion Disks MCG-6-30-15 (Tanaka et al.) Gravitational redshift plus Doppler shift Evidence that  ~  max = 1/2 m

20. 20 Do Jets Require an Accretion Disk? Yes “Interacting winds”, “ion torus”, Pulsars, need more work

21. 21 Do Accretion Disks Require Jets or Outflows? Are outflows/jets the main mechanism for transport/removal of angular momentum (Königl; Pudritz & Norman ’86; Li ’96)? Angular momentum carried by wind

22. 22 Do Accretion Disks Require Jets or Outflows? Angular momentum that needs to be removed from disk For r A ~ 10r, only 1% of the accreted mass needs to be lost in wind.

23. 23 Behavior of Disk Radius During Dwarf Nova Outburst At outburst, matter diffuses inward. Angular momentum of that matter is transferred to outer parts of the disk. Radius expands Observations OY Car, HT Cas, Z Cha (Harrop-Allin & Warner ’96) Disks in OY Car, HT Cas and Z Cha larger in outburst. U Gem Smak 1984

24. 24 Behavior of Disk Radius During Dwarf Nova Outburst Theory, disk instability Ichikawa & Osaki 1992; Livio & Verbunt 1988

25. 25 Do accretion disks require jets or outflows for angular momentum removal? I don’t think so. Observations of rotation in jets and bipolar outflows are badly needed (velocity gradients).

26. 26 Other Clues on Jets Jet Origin ObjectExampleV jet /V escape YSOsHH30, 34 V j ~ 100-350km/s V esc ~ 500km/s ~1 AGNM87; radio sources  >~ 3;  <~ 10 ~1 GRBs  ~ 100 ~1 XRBsSS 433; Cyg X-3 V j ~ 0.6c ~1 XRTsGRO 1655-40 GRS 1915+105 V j >~ 0.9c ~1 PneFliers, Ansae V ~ 200km/s ~1 SSS0513-69 V j ~ 3800km/s ~1

27. 27 Jets originate from the center of the accretion disk! Models which work at all radii are probably not the “correct” ones, (e.g. self similar).

28. 28 Black Hole Jets Two states: (i)dissipation and disk luminosity, (ii)bulk flow and jet. Livio, Pringle, King 2003, 2004; Mirabel 1993, 1998; Fender 2003; Fabian 2002, 2003

29. 29 New Timescale Timescale for jet t j ~ t d 2 R/H 1/f power spectrum below a break frequency. King, Pringle, West, Livio 2004 Hujeirat, Livio, Camenzind, Burkert 2003

30. 30 Which ingredients play a major role in the acceleration and collimation?

31. 31 Ingredients which may not be absolutely necessary YSOsAGNXRBsSSSPne(CVs) Central object near break-up rotation No?No, ??No? Relativistic central object NoYes No “Funnel”No (?) NoYes (?)No L >~ L Edd (Radiation pressure) (wind can be driven; Murray et al. 1997) No Yes No Extensive hot atmosphere (gas pressure) Yes (?)YesNo Yes (?)No Boundary layerYes (?)No?Yes (?)

32. 32 What Does Work? A reasonably ordered large-scale magnetic field threading the disk!

33. 33 Magneto-Centrifugal Jet Acceleration and Collimation 1.Acceleration like a bead on a wire up to the Alfven surface. 2.Acceleration optimal around inclination of 60° (Blandford & Payne 1982; Meier et al. 1997).

34. 34 Collimation Outside Alfven Surface Collimation by hoop stress? BUT Kink Instability Heyvaerts & Norman 1996

35. 35 Poloidal Collimation Necessary Conditions 1. R disk /R object = Significant number of decades 2. B z largest at inner disk but largest at outer disk e.g. B z ~ (r/R in ) -1 Good collimation obtained for R Alfven ~ R disk Konigl & Kaatje 1994; Spruit 1996 Consequences Minimum opening angle of jet  min ~ (R in /R out ) 1/2

36. 36 M87 Junor, Biretta, Livio 1999

37. 37

38. 38 Relativistic Outflow Magnetic flux tubes across horizon propel relativistic outflow. No collimation Koide 2004

39. 39 Are There Additional Ingredients? 1.Why are there radio-loud and radio-quiet AGN? 2.Why do CVs appear not to produce jets while PNe nuclei and SSS do? 3.How can pulsars produce jets?

40. 40 Conjecture The production of powerful jets requires an additional heat/wind source. Solutions to transsonic flow in disk corona (Ogilvie & Livio 1997, 2000)  for strong B a potential difference exists even for i > 30 (  ~ B 4 ).

41. 41 Energy Extraction from Spinning Holes Penrose Process –Negative energy orbits within “ergosphere”. –Need fortuitous collision or deus ex machina. Electromagnetic Extraction –Magnetic fields supported by external current interacts with “conducting” horizon. –Energy extracted to jet and disk. –Corotating observer sees energy flow across horizon. –Conserved outward flow of energy, angular momentum in non-rotating frame. –Reduce m; increase m 0.

42. 42 Radio Loud vs. Radio Quiet AGN Sikora et al. 2006 Xu, Baum & Livio 1999 Rawlings 1994 Central engine parameters:

43. 43 Spins of Black Holes? R ISCO, a *, determined on the basis of x-ray data. Study of plunging orbits important. McClintock et al. 2006 Shafee et al. 2006 Zhang, Cui & Chen 1997 Source M (M ʘ ) a*a* 1655-406.3+-.27~0.7 1543-479.4+-1.0~0.8 1915+10514+-4.4>0.98

44. 44 Critical Observations For the General Picture 1.Reliable determinations of 2.Determinations of the collimation scale in all classes of objects. 3.Long-term monitoring for variablity patterns in double-peaked emission lines in AGN. Power spectra. 4.Detection and measurement of rotation and of toroidal magnetic fields in jets and bipolar outflows. 5.More evidence for precession. 6.Breaks in afterglows of GRBs.

45. 45 Critical Observations For the Conjecture 1.Searches for jets in other SSS, in PNe, in other XRTs (during flares, e.g. A0620-00, GS2023+338, GS 1124-683, Cen X-4, AQL X- 1), and other symbiotic systems, in CVs! 2.Determination of black hole masses in AGN. 3.Determination of black hole spins in AGN (e.g., through Fe K  line profiles). 4.Determination of black hole spins in stellar mass black holes. 5.Determine whether pulsars can generate highly collimated jets.