Transcript MICROQUASARS

Radio Cores: Particle Accelerators
and High-Energy Laboratories
adopted from:
K. M annheim
(1998)
VLBI: Krichbaum et al. (1999)
Courtesy Heino Falcke
•TeV neutrinos
•511 keV annihilation line
•Gamma-rays
Spectrum of a Quasar
Jets are the only truly broad-band sources in the universe (radio-TeV)!
thermal
(disk)
Synchrotron
inverse Compton
(jet)
(jet)
Lichti et al. (1994)
HARD X-RAYS IN COMPACT mQSO JETS ?
Not new …
Shakura & Sunyaev (1973)
X-RAY & GAMMA-RAYS FROM
MICROQUASAR JETS
In conical jets: Size a 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)
MICROBLAZARS
(Mirabel & Rodriguez, ARAA 1999)
relativistic beaming: Dt a 1/2g2 ;
Due to
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.)
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 Q < 10o  transient lasting a few hours
UNIDENTIFIED EGRET SOURCES (>100 MeV)
TWO GALACTIC SUBSAMPLES:
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)
ULTRALUMINOUS X-RAY SOURCES
X-ray (Chandra)
Antennae
SUPER-EDDINGTON X-RAY SOURCES
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 ?
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)
GRBs & MICROQUASARS
BH PARADIGM
MICROQUASARS: JETS DURING TRANSIENT ACCRETION
G= 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 ?
A UNIVERSAL MECHANISM
Microblazar
Blazar
GRB
(Mirabel & Rodriguez; Sky & Telescope, May 2002)
QPOs IN MICROQUASARS
XTE & INDIAN SAT.
GRS 1915+105 (Strohmayer)
•Maximum fix frequencies of 40 & 67 Hz repeat
•This 3:2 ratio now found in 5 BHXBs (Remillard et al.) 
J. Rodriguez
must depend on fundamental properties of black hole
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.)
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
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
PARIS
IN GALACTIC & EXTRAGALACTIC
HIGH ENERGY ASTROPHYSICS
SACLAY
CONTACT:
[email protected]
INTEGRAL WILL BE LAUNCHED
IN OCTOBER 17, 2002
MULTIWAVELENGHT INTEGRAL NETWORK (“MINE”)
Contact person: Yael Fuchs
[email protected]