Astrophysical JetsMario Livio Space Telescope Science Institute

Which Systems Have Highly Collimated Jets?StellarExtragalactic

Object Physical SystemYoung Stellar ObjectsAccreting StarHMXBsAccreting NSX-ray TransientsAccreting BHLMXBsAccreting NSSupersoft X-ray SourcesAccreting WDSymbiotic starsAccreting WDPulsars (?)Rotating NSPlanetary NebulaeAccreting Nucleus or Interacting Winds

ObjectPhysical SystemAGNAccreting Supermassive BHGRBsAccreting BH

Disks around Young Stars STScI-PRC99-05b

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

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

Superluminal sourcesGRS 1915+105 V ~ 0.9cExtragalactic jets show V > 0.995c

Gamma Ray BurstsFruchter et al. 2006

SymbioticsSouthern Crab Nebula He2-104STScI-PRC99-32

Planetary Nebulae STScI-PRC97-38b

Point-Symmetric Planetary NebulaeIC 4634

Point-Symmetric Planetary Nebulae

Point-Symmetric Planetary Nebulae

SS 433Vermeulen et al. 1993

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

Recurrent Novae and SymbioticsU Sco (1999)Lpine, Shara, Livio & Zurek 1999Hillwig, Livio & Honeycutt 2004

Pulsar JetsChandraCrab PulsarVela PulsarChandra

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?)SSSYesH/LMXBsYesBHXTsYesGRBsWe dont knowAGNYes (?) (but maybe ion torus and surrounding gas pressure? Fabian & Rees 1995)

[OI] l6300 Profiles for T Tauri StarsRedshifted component not seen because of disk.Edwards et al. 1987Livio & Xu 1997

X-Ray Spectroscopy of Accretion DisksMCG-6-30-15 (Tanaka et al.)Gravitational redshift plus Doppler shiftEvidence that ~ max = 1/2 m

Do Jets Require an Accretion Disk?YesInteracting winds, ion torus, Pulsars, need more work

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

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

Behavior of Disk Radius During Dwarf Nova OutburstAt outburst, matter diffuses inward. Angular momentum of that matter is transferred to outer parts of the disk.Radius expandsObservationsOY Car, HT Cas, Z Cha (Harrop-Allin & Warner 96)Disks in OY Car, HT Cas and Z Cha larger in outburst.U GemSmak 1984

Behavior of Disk Radius During Dwarf Nova OutburstTheory, disk instabilityIchikawa & Osaki 1992; Livio & Verbunt 1988

Do accretion disks require jets or outflows for angular momentum removal?I dont think so.

Observations of rotation in jets and bipolar outflows are badly needed (velocity gradients).

Other Clues on JetsJet Origin

ObjectExampleVjet/VescapeYSOsHH30, 34Vj ~ 100-350km/sVesc ~ 500km/s~1AGNM87; radio sources g >~ 3; g ~ 0.9c~1PneFliers, Ansae V ~ 200km/s~1SSS0513-69 Vj ~ 3800km/s~1

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).

Black Hole JetsTwo states: dissipation and disk luminosity, bulk flow and jet.Livio, Pringle, King 2003, 2004; Mirabel 1993, 1998; Fender 2003; Fabian 2002, 2003

New TimescaleTimescale for jet tj ~ td2R/H1/f power spectrum below a break frequency. King, Pringle, West, Livio 2004 Hujeirat, Livio, Camenzind, Burkert 2003

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

Ingredients which may not be absolutely necessary

YSOsAGNXRBsSSSPne(CVs)Central object near break-up rotationNo?No, ??No?Relativistic central objectNoYesYesNoNoNoFunnelNo (?)No (?)No (?)NoYes (?)NoL >~ LEdd (Radiation pressure) (wind can be driven; Murray et al. 1997) NoNoNoYesYesNoExtensive hot atmosphere (gas pressure)Yes (?)YesNoNoYes (?)NoBoundary layerYes (?)No?Yes (?)Yes (?)Yes (?)

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

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

Collimation Outside Alfven SurfaceCollimation by hoop stress?BUTKink InstabilityHeyvaerts & Norman 1996

Poloidal CollimationNecessary Conditions Rdisk/Robject = Significant number of decades Bz largest at inner disk but largest at outer disk e.g. Bz ~ (r/Rin)-1Good collimation obtained for RAlfven ~ RdiskKonigl & Kaatje 1994; Spruit 1996

ConsequencesMinimum opening angle of jet min ~ (Rin/Rout)1/2

M87Junor, Biretta, Livio 1999

Relativistic OutflowMagnetic flux tubes across horizon propel relativistic outflow. No collimation Koide 2004

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

ConjectureThe 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 (Df ~ B4).

Energy Extraction from Spinning HolesPenrose ProcessNegative energy orbits within ergosphere.Need fortuitous collision or deus ex machina.Electromagnetic ExtractionMagnetic 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 m0.

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

Spins of Black Holes?RISCO, a*, determined on the basis of x-ray data.Study of plunging orbits important.McClintock et al. 2006Shafee et al. 2006Zhang, Cui & Chen 1997

SourceM (M)a*1655-406.3+-.27~0.71543-479.4+-1.0~0.81915+10514+-4.4>0.98

Critical ObservationsFor the General PictureReliable determinations of Determinations of the collimation scale in all classes of objects.Long-term monitoring for variablity patterns in double-peaked emission lines in AGN. Power spectra.Detection and measurement of rotation and of toroidal magnetic fields in jets and bipolar outflows.More evidence for precession.Breaks in afterglows of GRBs.

Critical ObservationsFor the ConjectureSearches 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!Determination of black hole masses in AGN.Determination of black hole spins in AGN (e.g., through Fe Ka line profiles).Determination of black hole spins in stellar mass black holes.Determine whether pulsars can generate highly collimated jets.