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MICROQUASARS

MICROQUASARS. Felix Mirabel European Southern Observatory Santiago, Chile. THE IDEA OF MICROQUASAR. Mirabel, Rodriguez, et al, 1992. Wang et al. ApJ 2002. Chandra. Belanger, Goldwurm, Goldoni, ApJ 2003. INTEGRAL. Black Hole. QUASAR-MICROQUASAR ANALOGY.

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MICROQUASARS

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  1. MICROQUASARS Felix Mirabel European Southern Observatory Santiago, Chile

  2. THE IDEA OF MICROQUASAR Mirabel, Rodriguez, et al, 1992 Wang et al. ApJ 2002 Chandra Belanger, Goldwurm, Goldoni, ApJ 2003 INTEGRAL Black Hole

  3. QUASAR-MICROQUASAR ANALOGY QUASAR MICROQUASAR Mirabel & Rodriguez; Nature 1992, 94, 98 The scales of length and time are proportional to MBH Rsh = 2GMBH/c2 ; DT a MBH The maximum color temperature of the accretion disk is: Tcol a (M/ 10M)-1/4 (Shakura & Sunyaev, 1976) For a given accretion rate: LBol a MBH ; ljeta MBH ; j a MBH-1 ; B a MBH-1/2 (Sams, Eckart, Sunyaev, 96; Rees 04) APPARENT SUPERLUMINAL MOTIONS IN mQSOs AS IN QSOs ?

  4. SUPERLUMINAL EJECTION IN A mQSO Mirabel & Rodriguez, 1994 THE PLASMA THAT RADIATES IN THE HARD X-RAYS IS BLOWN IN SUPERLUMINAL JETS VLA l3.6 cm 1 arcsec Vapp = 1.3c for a DISTANCE = 12 Kpc

  5. Mirabel & Rodriguez, 1994 WITH SAME BULK LORENTZ FACTORS SUPERLUMINAL MOTIONS IN AGN & mQSOs • MOVE ON THE PLANE OF THE SKY ~103 TIMES FASTER • JETS ARE TWO-SIDED WHICH ALLOWS TO SOLVE EQUATIONS • BETTER AGN AT <100 Mpc. e.g. Collimation @ 30-100 Rsh in M87 (Biretta)

  6. DT a MBH Mirabel et al. Nature 98; using RXTE + ESO + NRAO ACCRETION–JET CONNECTION • INFRARED & RADIO SYNCHROTRON EMISSION FROM THE JETS • JETS APPEAR ~5 MIN AFTER DISAPPEARANCE OF THE INNER DISK • THE ONSET OF THE JET IS AT THE TIME OF A “SPIKE” IN THE X-RAYS: SUDDEN REBUILT OF THE INNER DISK & LAUNCH A SHOCK THROUGH

  7. COMPACT STEADY JETS Ribo, Mirabel, Dhawan 2005 Mirabel et. al, 1998 2.0 cm 3.6 cm • ~100 AU IN LENGTH PRESENT DURING PLATEAU STATE • SPEED OF THE FLOW < 0.4c (Ribo, Mirabel & Dhawan 2005) • LARGE SCALE JETS ARE SHOCKS PROPAGATING AT ~0.98c • THROUGH THE SLOWER MOVING COMPACT JET • THE COMPACT JET REAPPEARS HOURS AFTER FLARES

  8. ANALOGOUS ACCRETION-JET CONNECTION IN THE SCALE-UP mQSO3C 120Marscher, Gomez, et al. Nature 2002 Red: X-rays Yellow: Radio

  9. DARK JETS FROM BLACK HOLES (Dubner et al) X-rays: (Brinkmann et al) SS433/W50 VLA l20cm 1o = 60 pc 1arcsec • ATOMIC NUCLEI MOVING AT 0.26c  • MECHANICAL LUMINOSITY > 1040 erg/sec • NON RADIATIVE JETS = “DARK” JETS

  10. LARGE-SCALE JETS IN GRS 1915+105(TRIGGERING STAR FORMATION ?) Rodriguez & Mirabel, 2000 VariableNT feature ?

  11. OTHER LARGE-SCALE JETS ? Cyg X-1 ( Gallo et al. Nature 2005) Cyg X-3 (Marti et al.2005) >50% OF THE RELEASED ENERGY IS NOT RADIATED

  12. MOVING X-RAY JETS IN A mQSO mQSOs XTE J1550-564 & H1743-322 Corbel et al. (2002, 05) X-rays are produced by synchrotron  electrons accelerated to TeV energies

  13. MICROBLAZARS(Mirabel. & Rodriguez, ARAA 1999) Due to relativistic beaming: Dt a 1/2g2 ; I a 8g3 e.g. If g = 5, Q< 10o Dt < 1/50 and DI > 103 SHOULD APPEAR AS SOURCES WITH FAST AND INTENSE VARIATIONS OF FLUX  DIFFICULT TO FOLLOW AND TO FIND mblazars from HMXBs may appear as variable gamma-ray sources due to Inverse Compton on UV photons of donor (Romero, Kauffman, Mirabel 2002; Bosch-Ramon & Paredes, 2004)

  14. Paredes et al. 2004 HAVE TWO MICROBLAZARS BEEN FOUND ? • Both inside EGRET error box (MeV-GeV) • LS 5039 has HESS counterpart >100 GeV • (Aharonian et al. Science 2005) • Both are massive stars in eccentric orbits • around compact objectsof< 4 M • Both are young runaway compact binaries • (Ribo et al. 2002; Mirabel & Rodrigues 2004) • X-ray time variability supports scenario of • jets fed by disks (Massi; Bosch-Ramon et al. 2005) LS 5039 LS 5039 LSI +61 303 Massi et al.04 Alternative model: Relativistic wind from young pulsar e.g.: PSR B1259-63 in HMXB detected by HESS at periastron

  15. HOW ARE BLACK HOLE BINARIES FORM ? THERE ARE THEORETICAL MODELS e.g. Fryer & Kalogera ; Woosley & Heger (2002) BUT FEW OBSERVATIONS ! • Mirabel & I. Rodrigues (2001-05) used the kinematics of mQSOs to find out: • BIRTH PLACE & NATURE OF THE PROGENITOR STARS • WHETHER THE PROGENITOR STAR ALWAYS EXPLODES AS AN ENERGETIC SUPERNOVAE

  16. GAMMA-RAY BURSTS OF LONG DURATION MARK THE BIRTH OF BLACK HOLES AT COSMIC DISTANCES Association with JETS, SN Ic & GRB @ Z=6.4  PROGENITORS OF GRB’s ARE MASSIVE BINARIES SOME mQSOs ARE FOSSILS OF GRBs

  17. RUNAWAY BLACK HOLE Mirabel, Irapuan Rodrigues et al. (A&A 395, 595, 2002) Proper motion with HST + radial velocity from ground RUNAWAY VELOCITY ~120 km/s MOMENTUM = 550 M km/s as in runaway neutron stars A LIKELY FOSSIL OF A GRBs FORMED IN AN HYPER-NOVA (Israelian et al. Nature 2001) GRO J1655-40 MBH ~ 4 M ORBITS FOR THE LAST 230 Myrs Yellow: Sun White: BH binary LOW-MASS BLACK HOLE FORMED IN A LUMINOUS SUPERNOVA

  18. THE HIGH MASS BLACK HOLE IN Cyg X-1 FORMED IN THE DARK Mirabel & Rodrigues, Science (2003) V < 9 +/- 2 km/s  < 1 M ejectedin SN Otherwise it would have shot out from the parent association MBH > 10 M MASSIVE STELLAR BH’s FORM PROMPTLY ?

  19. A BLACK HOLE FORMED ~7 BILLONS YEARS AGO IN THE GALACTIC HALO GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs Yellow: Sun White: BH binary Mirabel, Rodrigues et al. Nature, 2001 XTE J1118+480 MBH = 9 M l=158o b=+62o; D=1.9 kpc GALACTIC ARCHEOLOGY OF MASSIVE STARS PROBABLY ONE OF THE SEVERAL MILLONS BHs THAT ESCAPED FROM GLOBULAR CLUSTERS

  20. THE mQSO/AGN ANALOGY IS CONFIRMED AND MAY BE USED TO GAIN KNOWLEDGE IF THE PHENOMENOLOGICAL CORRELATIONS mQSO/AGN 1) X-ray/radio/mass, 2) QPOs/mass, 3) Noise-spectrum/mass became robust, independently of the models ESTIMATE THE MASS OF BLACK HOLES ANALOGOUS SITUATION OF H-R DIAGRAM IN STELLAR ASTRONOMY

  21. Fe Ka LINES IN mQSOs Cygnus X-1 Miller et al. (2002) FOUND IN ~6 MICROQASARS • CHANDRA, XMM & Beppo-SAX • Asymmetry: gravitational redshift, • Doppler & transverse-Doppler shift • Narrow component from outer disk ? • Broad component from inner disk • SPINNING BLACK HOLE? mQSOs MAY BE GOOD LABORATORIES TO STUDY IN SHORT TIME SCALES THE Fe Ka LINES AS A FUNCTION OF X-RAY STATE TO TEST MODELS ON THE ORIGIN OF THESE LINES IN SEYFERTS

  22. QSO - mQSO -GRB ANALOGY HAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, S&T 2002) neutron star no ? no AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?

  23. CONCLUSION Microquasars have provided insight into: • THE PHYSICS OF RELATIVISTIC JETS FROM BH’s • THE CONNECTION BETWEEN ACCRETION & EJECTION • THE FORMATION OF STELLAR-MASS BLACK HOLES • Microquasars could provide insight into: • A LARGE FRACTION OF ULXs IN NEARBY GALAXIES • GRBs OF LONG DURATION IN DISTANT GALAXIES

  24. X-RAY - RADIO CORRELATIONS IN LOW-POWER BHs OF ALL MASSES Radio-X-ray correlation in low-hard state mQSOs (Corbel et al. 02; Gallo, Fender & Pooley, 03; Maccarone et al.03) The power output of quiescent BHs is jet-dominated In high-soft X-ray state the radio jets are quenched. Also in AGN. Sgr A*, LINERs, FR I & BL Lac are analogous to mQSOs in the low-hard state(Falcke,et al. 04) Relation between X-ray, radio & mass of BHs 5 GHz & 2-10 keV core emission (Merloni, Heinz & Di Matteo 03) From radiativelly inefficient accretion rather than thin synchrotron Radio/bolometric luminosity larger in AGN (Heinz & Sunyaev 2003) If more robust, independently of the model THE MASS OF BLACK HOLES COULD BE INFERRED

  25. TIME VARIATIONS SEEM TO SCALE WITH BLACK HOLE MASS 1) Duration of X-ray flares in Cyg X-1 and Sgr A* In Cyg X-1 and other BHXRBs: 1-10 ms (Gierlinski & Zdziarski, 03) In Sgr A* 400-10,000 s(Baganoff et al. 01; Goldwurm et al. 03) 2) 3:2 twin peak kHz QPO in mQSOsand the spin of BHs In 3 mQSOsa = J/(GM/c2) = 0.6-0.9(Remillard 2004) Due to gravitational cyclic modes (Abramowicz et al. 2004) Observations in Sgr A* : IR QPOs of ~17 min a = 0.52(Genzel et al. Nature. 04) X-ray QPOs that include twins of 12 & 19 min (Aschenbach et al. 04). Strohmayer GRS 1915+105 DT ratio ~ MSgrA BH / Mstellar BH = 105-6 Independently of the model The BH mass in ULXs may be derived

  26. APERIODIC VARIABILITY IN AGN & mQSOs • The break time scale in the power spectral density of black holes seems to scale linearly with the mass of the BH (Uttley & McHardy, 2001) • The NLS1 NGC 4051 scales better with Cyg X-1 in the soft-high state (Lbol ~ 0.3 Ledd) • The broad band Sey 1 NGC 3516 scales linearly • with Cyg X-1 in the low-hard state (McHardy, 04) • Most of the aperiodic variation in Cyg X-1 is due to the harder component (Churazov, Gilfanov, Revnivtsev, 2001) • Propagating perturbations in the accreting flow (Uttley, 2004) THE MASS OF BLACK HOLES IN ULXs COULD BE DETERMINED

  27. XTE & INDIAN SAT. QPOs AND GENERAL RELATIVITY GRS 1915+105 (Strohmayer) • High frequency QPOs (e.g. 40 & 67 Hz repeat in GRS) • This 3:2 ratio now found in 4 BHXBs (Remillard et al.)  • must depend on fundamental properties of black hole Tagger; Chakrabarti, Zhang nmax = f(MBH, Spin) DETERMINE THE SPIN OF BLACK HOLES THE BH SPIN & DISK TEMPERATURE SUGGEST THAT JETS MAY BE POWERED BY THE BH SPIN(Zhang et al.; Wang)

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