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

Synchrotron(jet)

Synchrotron(jet)

thermal(disk)

thermal(disk)

inverse Compton(jet)

Lichti et al. (1994)

Jets are the only truly broad-band sources in the universe (radio-TeV)!Jets are the only truly broad-band sources in the universe (radio-TeV)!

HARD X-RAYS IN COMPACT QSO JETS ?Not new …

Shakura & Sunyaev (1973)Shakura & Sunyaev (1973)

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

By inverse Compton may be sources of gamma-rays (Aharonian & Athonian 1999)

In conical jets: Size -1

(Dhawan, Mirabel, Rodriguez 01)

MICROBLAZARS (Mirabel & Rodriguez, ARAA 1999)

Due to relativistic beaming: t

e.g. If = 5, t < 1/50 and I > 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.)

2) 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

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 transient lasting a few hours

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

X-ray (Chandra) Antennae

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 ChandraLx ~ 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

MICROQUASARS: JETS DURING TRANSIENT ACCRETION

= 2-10 E < 1047 erg. RECURRENT EJECTION EVENTS

GRBs: JETS DURING FORMATION OF STELLAR MASS BHs

= 200 E ~ 1052 erg . UNIQUE CATASTROPHIC EVENTS

BUT IN THE MOST RECENT COLLAPSAR MODELS

= 2-10 AT THE BASE OF GRB JETS

BH PARADIGM

A UNIVERSAL MECHANISM OF JET

FORMATION IN QSOs, AGNs AND GRBs ?

A UNIVERSAL MECHANISM

Microblazar Blazar GRB

(Mirabel & Rodriguez; Sky & Telescope, May 2002)

QPOs IN MICROQUASARSGRS 1915+105 (Strohmayer) XTE & INDIAN SAT.

max = 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 K LINES IN QSOsCygnus X-1 Miller et al. (2002)

CHANDRA, XMM & Beppo-SAX

•Narrow component from outer disk ?

•Broad component from inner disk

•IS IT VARIABLE GRS 1915+105 ?

( Lee et al. 2002; Martocchia et al. 2002)

QSOs MAY BE GOOD LABORATORIES TO STUDY IN SHORT TIME SCALES THE Fe KLINES 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:

• 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

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