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Radio Cores: Particle Accelerators and High-Energy Laboratories

Radio Cores: Particle Accelerators and High-Energy Laboratories. TeV neutrinos 511 keV annihilation line Gamma-rays. VLBI: Krichbaum et al. (1999) Courtesy Heino Falcke. thermal (disk). Synchrotron (jet). inverse Compton (jet). Spectrum of a Quasar.

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Radio Cores: Particle Accelerators and High-Energy Laboratories

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  1. Radio Cores: Particle Accelerators and High-Energy Laboratories • TeV neutrinos • 511 keV annihilation line • Gamma-rays VLBI: Krichbaum et al. (1999) Courtesy Heino Falcke

  2. thermal(disk) Synchrotron(jet) inverse Compton(jet) Spectrum of a Quasar Jets are the only truly broad-band sources in the universe (radio-TeV)! Lichti et al. (1994)

  3. HARD X-RAYS IN COMPACT mQSO JETS ?Not new … Shakura & Sunyaev (1973)

  4. X-RAY & GAMMA-RAYS FROM MICROQUASAR JETS In conical jets: Sizea n-1 (Dhawan, Mirabel, Rodriguez 01) IN LOW/HARD-STATE DIRECT SYNCHROTRON IS MORE POWERFUL IN MICROQUASARS (Falcke et al. 2002) MICROQUASAR JETS MAY CONTAIN ELECTRONS WITH G ~ 107 By inverse Compton may be sources of gamma-rays (Aharonian & Athonian 1999)

  5. 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 POSSIBLE MICROBLAZARS: 1) Cygnus X-1: source of emission up to few MeV(Hurley et al.; McConnell et al.) • V4641 Sgr: optical fluctuations in minutes and jets with Vapp > 10c (Hjellming et al. 2000; Orosz et al. 2001; Uemura et al.) • BOTH ARE BLACK HOLES IN HMXBs

  6. PRECESSING MICROBLAZARS Possible gamma-ray sources by inverse Compton of the electron jets and external photon fields Kaufman, Romero, Mirabel (A&A, 2002) Romero, Kaufman, Mirabel (A&A, 2002) • Cyg X-1 MAY BE A PRECESSING MICROBLAZAR • Possible gamma-ray transients confirmed by BATSE(Golenetskii et al. IAUC 7840) • One-sided jet with possible variable ejection angle (Stirling et al.) • V > 0.5c with Q < 10o  transient lasting a few hours

  7. TWO GALACTIC SUBSAMPLES: UNIDENTIFIED EGRET SOURCES (>100 MeV) 1) Relics from core-collapsed SN correlated with the tilted Gould Belt (Grenier, 1998;Gehrels et al. 2000) 2)Variable, soft and faint population at a scale high of ~2 kpc with a distribution of halo objects (Grenier, 2001) TWO MICROQUASARS IN THE ERROR BOX OF EGRET SOURCES: • LS 5039: A microquasar (Paredes et al. 2000) • LSI+61 303: X-Ray faint (Harrison et al. 2000)

  8. ULTRALUMINOUS X-RAY SOURCES X-ray (Chandra) Antennae

  9. SUPER-EDDINGTON X-RAY SOURCES M82 seen by Chandra • Lx ~ 1040 erg/sec when Eddington limit Lx ~ MBHx 1038 erg/s • INTERMEDIATE MASS BHs > 200 M? • claimed by NASA press releases. However: • Photon spectra similar to Galactic stellar-mass black holes • Mostly seen in starburst galaxies (e.g. The Antennae) • Where such Intermediate-mass BHs would accrete from ? • Why none was found in the Milky Way ? SHORT-LIVED HMXBs (MICROQUASARS) ? WITH BEAMED EMISSION(Mirabel & Rodriguez, 1999; King et al 2001) WITHOUT BEAMED EMISSION BUT MBH > 60 M(Pakul et al. 2002)

  10. GRBs & MICROQUASARS BH PARADIGM • MICROQUASARS: JETS DURING TRANSIENT ACCRETION • = 2-10 E < 1047 erg. RECURRENT EJECTION EVENTS GRBs: JETS DURING FORMATION OF STELLAR MASS BHs • G = 200 E ~ 1052 erg . UNIQUE CATASTROPHIC EVENTS BUT IN THE MOST RECENT COLLAPSAR MODELS • G = 2-10 AT THE BASE OF GRB JETS A UNIVERSAL MECHANISM OF JET FORMATION IN mQSOs, AGNs AND GRBs ?

  11. A UNIVERSAL MECHANISM Microblazar Blazar GRB (Mirabel & Rodriguez; Sky & Telescope, May 2002)

  12. XTE & INDIAN SAT. QPOs IN MICROQUASARS GRS 1915+105 (Strohmayer) • Maximum fix frequencies of 40 & 67 Hz repeat • This 3:2 ratio now found in 5 BHXBs (Remillard et al.)  • must depend on fundamental properties of black hole J. Rodriguez nmax = f(MBH, Spin)  DETERMINE THE SPIN OF BLACK HOLES (Zhang et al) AND TEST WHETHER JETS ARE POWERED BY BH SPIN (B-Z; Koide) PROBLEM: SEVERAL GR MODELS (Wagoner et al; Abramovicz et al.)

  13. Fe Ka LINES IN mQSOs Cygnus X-1 Miller et al. (2002) FOUND IN 4 MICROQASARS • CHANDRA, XMM & Beppo-SAX • Narrow component from outer disk ? • Broad component from inner disk • IS IT VARIABLE IN GRS 1915+105 ? • ( Lee et al. 2002; Martocchia et al. 2002) 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

  14. CONCLUSION Microquasars allow to gain insight into: • THE PHYSICS OF RELATIVISTIC JETS • EVIDENCES FOR HORIZON  BLACK HOLE • THE CONNECTION BETWEEN ACCRETION DISK INSTABILITIES AND THE FORMATION OF JETS • CONSTRAIN THE ORIGIN AND EVOLUTION OF BHs NEW PERSPECTIVES • DETERMINE THE SPIN OF BLACK HOLES • GAIN INSIGHT INTO SUPERLUMINAL X-RAY SOURCES • GAIN INSIGHT INTO GRB AFTERGLOWS • SOURCES OF GAMMA-RAYS AND TeV NEUTRINOS ?

  15. POSSIBILITY OF COLLABORATIONS FOR STUDENTS, POST-DOCS & PROFESSORS IN GALACTIC & EXTRAGALACTIC HIGH ENERGY ASTROPHYSICS CONTACT: fmirabel@cea.fr PARIS SACLAY INTEGRAL WILL BE LAUNCHED IN OCTOBER 17, 2002 MULTIWAVELENGHT INTEGRAL NETWORK (“MINE”) Contact person: Yael Fuchs yfuchs@discovery.saclay.cea.fr

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