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David Vs. Goliath: What Accreting Stellar Mass Black Holes Can Teach Us About the Supermassive

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David vs. goliath: What accreting Stellar mass black holes can teach us about the supermassive S e r a M a r k o f f (API, University of Amsterdam) Outline Introduction, big picture, jargon Little black holes ⇔ supermassive? Evidence for mass-scaling physics, example applications Works in progress, and outlook/ summary Accretion (Gravitational Capture) V ra 1 GMm Jet mv2 = From ra inwards: 2 r Accretion Disk 2GM r = a v2 Jets form in many astronomical objects SUPERMASSIVE BLACK HOLES STELLAR-MASS BLACK HOLES FORMING STARS Cygnus A GRS 1915+105 HH 47 DYING STARS Cas A PN M2-9 Text GRB DEAD STARS R AQUARII CRAB PULSAR SS 433 Enormous effect on the local environment ~ 600k light years across! (McNamara et al. 2005) Enormous effect on the local environment Can actually stunt the growth of the host galaxy! Very important for galaxy evolution/cosmology. Also interested in the first black holes/ XRBs: epoch of reionization. (McNamara et al. 2005) Jets are likely the most powerful cosmic accelerators: AUGER 1st results We need a much better theoretical understanding of jet physics! What’s inside them? How and why are jets launched and confined? Requires more information about conditions near jet/disk interface: accretion flow “type” and geometry, balance of energy between magnetic fields and plasma, plasma content Enter the David vs. Goliath metaphor Jet X-ray Binary: Black hole/Neutron star compact corona Donor star Active Galactic Nucleus (Jets optional) Accretion disk corona Accretion disk 7-9 MBH ~ 10 M☉ MBH ~ 10 M☉ Black holes have no “hair” (J. Wheeler) ✸Is BH accretion (roughly) generic? —GR: shape of spacetime around BH determined only by M and a=Jc/GM2 (between 0-1) 2 —Kerr metric (rs=2GM/c ): rs 2rsa c2dτ 2 = 1 − c2dt2 + cdtdφ− ! r " # rc $ 2 −1 2 2 rs a a rsa 1 − + dr2 − 1+ + r2dφ2 ! r r2c2 " ! r2c2 r3c2 " ➠ If yes, physics of accretion should scale predictably between stellar and supermassive black holes ➠ Two scales: mass and accretion rate (power) ➠ CAVEAT: Accretion from one star vs. accretion from many stars + mergers seems pretty different... And yet...they look pretty similar! QUASAR (AGN) MICROQUASAR (XRB) 104-5 yrs! 1 day (Mirabel et al. 92,98) (Mirabel et al. 92,98) Time variable X-ray binary (XRB) behavior: The Hardness-Intensity Diagram (HID) Time variable XRB behavior: The HID Spectrum and Interpretation (Done, Gierlinski & Kubota 2007) Time variable XRB behavior: The HID Real data with states indicated Time variable XRB behavior: The HID What are the jets doing? Hard state: HIM/SIM transition = steady jets = ballistic jets Soft state: = no jets How can we test if this variability relates to the supermassive black holes in AGN? Mass scaling makes testable predictions The main effect of black hole mass difference will be in the timescales, τdyn ∝ size ∝ M: τXRB ∼ week @ 10 M☉ 6 8 τAGN ∼ 10 years @ 10 M☉ !! We can test this idea by searching for trends from individual XRB studies in AGN populations (ensembles) If such scaling exists, some AGN classes could be “unified” in a HID of their own ➠ also useful for evolution schemes Mapping XRB states ⇔ AGN classes? Radio (Loud) Galaxies ? ? LLAGN (Sgr A*, M81*, NGC4258) ? Seyferts/ Radio Quiet Quasars? First mapping established: “hard” state XRBs with Low-luminosity AGN Strong evidence both theoretically, and empirically: “Fundamental plane of black hole accretion” linking radio and X-ray luminosities with black hole mass Same physical models fit the data (well) over 7 orders of magnitude in mass, with the same physical parameters XRB hard state -- Universal Radio/X-ray Correlation Prediction of jet synchrotron model (Corbel et al. 2000, 2003; Markoff et al. 2003) “Traditional” Hard State SED components Fν Companion Accretion Jet Star Disk Corona Disk ▲▲▲▲▲▲▲▲▲▲ ✜✜✜✜✜ ➞ Radio to IR/opt ➞ ✜✜✜✜✜ ➞ Opt/UV/soft X-ray ➞ Hard X-rays ν Break frequency (normalization) scales with mass Fν 2/3 -1 νbreak ∝ Qjet M AGN: XRBs: radio IR/opt ▲▲▲▲▲▲▲▲ ✜✜✜✜✜✜ ✜✜✜✜✜✜ Expect same radio/X-ray correlation slope but AGN will have lower “normalization” in X-ray luminosity, comparatively! ν Fundamental plane of BH accretion Observed Merloni et al. 2006, Kording 2006) Falcke, Körding & Markoff 2004, 2005, (Markoff et al. 2003, Merloni,Heinz & diMatteo Mass “corrected” Modeling weakly accreting black holes Radio Synchrotron zacc,p,pl%,ξ IR/opt/ X-rays X-rays r0,Nj,Te, SSC/EC k=partition Modeling weakly accreting black holes Radio NIR OPT UV X-rays Stellar 0 1 Companion ! keV 2 ! 11 cm 1 ! 0.1 keV Photons s 0.01 024 C 2 ! 4 ! 10 !8 10 !7 10 !6 10 !5 10 !4 10 !3 0.01 0.1 110 100 Energy (keV) (Markoff et al. 04-07) XRBs: modeling simultaneous broadband data Migliari et al. 07, Gallo Maitra 08) 05, (Markoff et al. 03, Markoff, Nowak & Wilms M81*: nearby AGN hard state equivalent? All observations (Markoff et al. 2008) Sgr A*− Oddball black hole? M81* NGC 4258 NGC 4258 M81 Flares Sgr A* Quiescence Sgr A* GX 339-4 (Markoff 2005) Sgr A*− consistent with XRB hysteresis? NGC 4258 GX 339-4 (Corbel & Coriat, in prep.) Sgr A*: decomposing the system (Markoff, Bower & Falcke 2007, Doeleman (Markoff, & Falcke et al. 2008, Falcke, Bower Markoff 2009, Maitra, Markoff& Bower in prep.) & Falcke, With the latest radio global interferometry techniques, we can now almost image the event horizon! (factor of ∼3 to go) Sgr A*: decomposing the system (Markoff, Bower & Falcke 2007, Doeleman (Markoff, & Falcke et al. 2008, Falcke, Bower Markoff 2009, Maitra, Markoff& Bower in prep.) & Falcke, With the latest radio global interferometry techniques, we can now almost image the event horizon! (factor of ∼3 to go) Sgr A*: decomposing the system (Markoff, Bower & Falcke 2007, Doeleman (Markoff, & Falcke et al. 2008, Falcke, Bower Markoff 2009, Maitra, Markoff& Bower in prep.) & Falcke, With the latest radio global interferometry techniques, we can now almost image the event horizon! (factor of ∼3 to go) Sgr A*: decomposing the system (Markoff, Bower & Falcke 2007, Doeleman (Markoff, & Falcke et al. 2008, Falcke, Bower Markoff 2009, Maitra, Markoff& Bower in prep.) & Falcke, With the latest radio global interferometry techniques, we can now almost image the event horizon! (factor of ∼3 to go) Other groups: mass scaling in timing features (Uttley, McHardy, et al.) 2 τB ∝MBH /Lbol What sorts of things are we learning? 8 ✴From fitting 10-10 M☉, we find that all low- luminosity BH sources share similar traits: ‣ Jets anchored in rather compact “coronae” (~5-10rg) ‣ For these weaker states, magnetic acceleration of the bulk plasma not required ‣ Energetics: cold proton/hot electron model works, p- acceleration still needs to be incorporated ‣ Plasma only slightly magnetically dominated ‣ Particle acceleration is efficient, and occurs at fairly stable location in jets (~10-100rg), except in Sgr A*/A0620? ☛ Can use as boundary conditions for improved MHD models, and for time dependent models of transitional, higher accretion rate states. Gives clues about jet launching and accretion. Cygnus X-1: trove of radio/X-ray data ✴ Over 10 years of bi-weekly, simultaneous monitoring with RXTE and Ryle radio, most recently with other X-ray instruments like XMM, Integral, Suzaku and Chandra (Wilms, Pottschmidt, Nowak, Pooley, Markoff, et al.) ‣ Beyond spectral and timing evolution, we are starting to resolve timescales between emission regions (e.g., Wilms et al. 2007): JD!2453476 0.63 0.64 0.65 0.66 0.67 80 0.4 RXTE PCA Rate [counts s 2500 0.3 60 2000 0.2 [mJy] 40 15 GHz 0.1 Scargle CCF F 1500 ! 1 20 PCU 0.0 ! 1 1000 ] 0 !0.1 3 4 !2000 !1000 0 1000 2000 2005 April 16 Time Lag [s] Cygnus X-1: Corona/jet relationship (Hanke et al. 2009) (Hanke Cygnus X-1: Corona/jet relationship II (Hanke et al. 2009, Nowak et al. 2009) et al. 2009, Nowak (Hanke Cygnus X-1: Corona/jet relationship II (Hanke et al. 2009, Nowak et al. 2009) et al. 2009, Nowak (Hanke Cygnus X-1: Corona/jet relationship III Single Two Eqpair Eqpair T (high) T’s (low) Jet + T/NT et al. 2009) (Nowak diskbb hybrid + Jet T (low) T (low) Radio/ IR Cygnus X-1: Corona/jet relationship IV Lepton number density Pair production rate Pair annihilation rate (Maitra, Markoff et al. 2009; Markoff, Pe’er & Maitra, in prep.) Modeling weakly accreting black holes Radio Synchrotron zacc,p,pl%,ξ IR/opt/ X-rays X-rays r0,Nj,Te, SSC/EC k=partition Developing jet internal dynamics (Vlahakis 2003,& Königl Polko--PhD, Markoff, Meier, Markoff, Meier, Polko--PhD, in prep.) Outward Modified Fast Point (MFP) integration Alfvén Point Inward integration Modified Slow Point (MSP) Accretion disk Black hole Developing jet internal dynamics (Vlahakis 2003,& Königl Polko--PhD, Markoff, Meier, Markoff, Meier, Polko--PhD, in prep.) Outward Modified Fast Point (MFP) integration Alfvén Point Inward integration Modified Slow Point (MSP) Accretion disk Black hole Developing jet internal dynamics (Vlahakis 2003,& Königl Polko--PhD, Markoff, Meier, Markoff, Meier, Polko--PhD, Outward Modified Fast Point (MFP) in prep.) integration Alfvén Point Inward integration Modified Slow Point (MSP) Accretion disk Black hole AGN ⇔ XRB mapping? Radio Galaxies ? LLAGN ? (Sgr A*, ? M81*, ➝ Seyferts/ NGC4258) Radio Quiet AGN? Luminosity Summary ✸ Little black holes behave remarkably like scaled down supermassive ones (not obvious astronomically speaking) ✸ Shorter timescales in XRBs make them extremely valuable for answering the “big” questions in accretion ✸ Already providing an important stepping stone for understanding the largest scale behavior: ➠ Some of the AGN “zoology” can be interpreted as very long- term evolution between XRB state analogs, with differnt driving mechanism (mergers, etc.) ➠ One “unification” so far: the steady, weakly accreting hard state XRBs and weakly accreting AGN ➠ Provided new clues about the role and geometry of the accretion flow and magnetic fields, plasma content, particle acceleration and more..
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  • Quasar Jet Emission Model Applied to the Microquasar GRS 1915+105

    Quasar Jet Emission Model Applied to the Microquasar GRS 1915+105

    A&A 415, L35–L38 (2004) Astronomy DOI: 10.1051/0004-6361:20040010 & c ESO 2004 Astrophysics Quasar jet emission model applied to the microquasar GRS 1915+105 M. T¨urler1;2, T. J.-L. Courvoisier1;2,S.Chaty3;4,andY.Fuchs4 1 INTEGRAL Science Data Centre, ch. d’Ecogia 16, 1290 Versoix, Switzerland 2 Observatoire de Gen`eve, ch. des Maillettes 51, 1290 Sauverny, Switzerland Letter to the Editor 3 Universit´e Paris 7, 2 place Jussieu, 75005 Paris, France 4 Service d’Astrophysique, DSM/DAPNIA/SAp, CEA/Saclay, 91191 Gif-sur-Yvette, Cedex, France Received 18 December 2003 / Accepted 14 January 2004 Abstract. The true nature of the radio emitting material observed to be moving relativistically in quasars and microquasars is still unclear. The microquasar community usually interprets them as distinct clouds of plasma, while the extragalactic com- munity prefers a shock wave model. Here we show that the synchrotron variability pattern of the microquasar GRS 1915+105 observed on 15 May 1997 can be reproduced by the standard shock model for extragalactic jets, which describes well the long-term behaviour of the quasar 3C 273. This strengthens the analogy between the two classes of objects and suggests that the physics of relativistic jets is independent of the mass of the black hole. The model parameters we derive for GRS 1915+105 correspond to a rather dissipative jet flow, which is only mildly relativistic with a speed of 0:60 c. We can also estimate that the shock waves form in the jet at a distance of about 1 AU from the black hole.
  • Relativistic Jets in Active Galactic Nuclei and Microquasars

    Relativistic Jets in Active Galactic Nuclei and Microquasars

    SSRv manuscript No. (will be inserted by the editor) Relativistic Jets in Active Galactic Nuclei and Microquasars Gustavo E. Romero · M. Boettcher · S. Markoff · F. Tavecchio Received: date / Accepted: date Abstract Collimated outflows (jets) appear to be a ubiquitous phenomenon associated with the accretion of material onto a compact object. Despite this ubiquity, many fundamental physics aspects of jets are still poorly un- derstood and constrained. These include the mechanism of launching and accelerating jets, the connection between these processes and the nature of the accretion flow, and the role of magnetic fields; the physics responsible for the collimation of jets over tens of thousands to even millions of gravi- tational radii of the central accreting object; the matter content of jets; the location of the region(s) accelerating particles to TeV (possibly even PeV and EeV) energies (as evidenced by γ-ray emission observed from many jet sources) and the physical processes responsible for this particle accelera- tion; the radiative processes giving rise to the observed multi-wavelength emission; and the topology of magnetic fields and their role in the jet colli- mation and particle acceleration processes. This chapter reviews the main knowns and unknowns in our current understanding of relativistic jets, in the context of the main model ingredients for Galactic and extragalactic jet sources. It discusses aspects specific to active Galactic nuclei (especially Gustavo E. Romero Instituto Argentino de Radioastronoma (IAR), C.C. No. 5, 1894, Buenos Aires, Argentina E-mail: [email protected] M. Boettcher Centre for Space Research, Private Bag X6001, North-West University, Potchef- stroom, 2520, South Africa E-mail: [email protected] S.