Clase4

Radio Cores: Particle Accelerators and High-Energy Laboratories: 

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

Spectrum of a Quasar: 

Spectrum of a Quasar Lichti et al. (1994) Jets are the only truly broad-band sources in the universe (radio-TeV)!

HARD X-RAYS IN COMPACT mQSO JETS ?Not new …: 

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

X-RAY & GAMMA-RAYS FROM MICROQUASAR JETS: 

X-RAY & GAMMA-RAYS FROM MICROQUASAR JETS 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) In conical jets: Size a n-1 (Dhawan, Mirabel, Rodriguez 01)

MICROBLAZARS (Mirabel & Rodriguez, ARAA 1999): 

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

PRECESSING MICROBLAZARS: 

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

UNIDENTIFIED EGRET SOURCES (>100 MeV): 

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

ULTRALUMINOUS X-RAY SOURCES: 

ULTRALUMINOUS X-RAY SOURCES Antennae

SUPER-EDDINGTON X-RAY SOURCES: 

SUPER-EDDINGTON X-RAY SOURCES 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) M82 seen by Chandra Lx ~ 1040 erg/sec when Eddington limit Lx ~ MBH x 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 ?

GRBs & MICROQUASARS : 

GRBs & MICROQUASARS 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 BH PARADIGM A UNIVERSAL MECHANISM OF JET FORMATION IN mQSOs, AGNs AND GRBs ?

A UNIVERSAL MECHANISM: 

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

QPOs IN MICROQUASARS: 

QPOs IN MICROQUASARS GRS 1915+105 (Strohmayer) 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.) 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

Fe Ka LINES IN mQSOs: 

Fe Ka LINES IN mQSOs Cygnus X-1 Miller et al. (2002) 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 FOUND IN 4 MICROQASARS

CONCLUSION Microquasars allow to gain insight into:: 

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 ?

POSSIBILITY OF COLLABORATIONS FOR STUDENTS, POST-DOCS & PROFESSORS: 

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