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MICROQUASARS
Felix Mirabel
European Southern Observatory. Chile
on leave from CEA-Saclay. France
Five international workshops
VI in Como, Italy (18-22 Sept. 2006)
HIGH ENERGY SOURCES IN THE GALACTIC CENTRE
Mirabel, Rodriguez, et al, 1992
Black Hole
Wang et al. ApJ 2002
Belanger, Goldwurm, Goldoni, ApJ 2003
INTEGRAL
Chandra
QUASAR-MICROQUASAR ANALOGY
The scales of length and time are proportional to MBH
Rsh = 2GMBH/c2 ; T MBH
Unique system of equations: The maximum color temperatureof the accretion disk is:
Tcol M/ 10M)-1/4
(Shakura & Sunyaev, 1976)Waited era of space astronomy
For a given accretion rate:
LBol MBH ; ljet MBH ;
MBH-1 ; BMBH
-1/2 (Sams, Eckart, Sunyaev, 96; Rees 04)
QUASAR MICROQUASAR Mirabel & Rodriguez (Nature 1998)
APPARENT SUPERLUMINAL MOTIONS IN QSOs AS IN QSOs ?
SUPERLUMINAL EJECTION IN A QSO
1 arcsec
Mirabel & Rodriguez, 1994
Vapp > C for a DISTANCE > 8 Kpc
cm
THE PLASMA THAT RADIATES IN THE HARD
X-RAYS IS BLOWN IN SUPERLUMINAL JETS VLA
GRS 1915+105
SUPERLUMINAL MOTIONS IN THE GALAXY
1) ASYMMETRIES DUE TO RELATIVISTIC ABERRATION IN TWIN JETS
2) QSOs HAVE SAME BULK LORENTZ FACTORS AS QSOs & BLAZARS
3) JET COLLIMATION @ 30-100 Rsh IN M87 IS CONSISTENT WITH THE
BLANDFORD-PAYNE MODEL (Biretta et al., 2004). HADRONIC JETS ?
DARK JETS FROM BLACK HOLESRadio (Dubner et al); X-rays: (Brinkmann et al)
SS433/W50
• ATOMIC NUCLEI MOVING AT 0.26c
• MECHANICAL LUMINOSITY > 1039 erg/sec
• NON RADIATIVE JETS = “DARK” JETS
• >50% OF THE ENERGY IS NOT RADIATED
1o = 60 pcarcsec
VLA 20cm
LARGE-SCALE JETS IN CYGNUS X-1
Gallo, Fender et al. Nature 2005
ring diameter = 5 pc
LARGE-SCALE JETS IN GRS 1915+105 ? Rodriguez & Mirabel (2006)
hot spots at ~ 50 pc
> 50% OF THE RELEASED
ENERGY IS NOT RADIATED
IS IT A VHE SOURCE ?
MOVING X-RAY JETS IN A QSOQSOs XTE J1550-564 & Corbel et al. Science 2002, 05
X-rays are produced by synchrotron electrons accelerated to TeV energies
ACCRETION–JET CONNECTION
- THE ONSET OF THE JET IS AT THE TIME OF A X-RAY “SPIKE” - SUDDEN REFILL OF THE INNER DISK & INJECTION INTO THE JETS - SHOCK THROUGH A MILDLY RELATIVISTIC COMPACT JET
T MBH Mirabel, Dhawan, Rodriguez (1998) 1 hr = 30 yr in SgrA*
GRS 1915+105
COMPACT STEADY JETS
• ~100 AU IN LENGTH PRESENT DURING PLATEAU STATE
• SPEED OF THE FLOW < 0.4c (Ribo, Dhawan & Mirabel 2005)
• LARGE SCALE JETS ARE SHOCKS PROPAGATING c
THROUGH THE SLOWER MOVING COMPACT JET
Ribo, Dhawan & Mirabel (2005) Mirabel, Dhawan, et al. 1998
2.0 cm 3.6 cm
GRS 1915+105
QSOs & ULTRALUMINOUS X-RAY SOURCES Microquasars in external galaxies
X-ray (Chandra) AntennaeFabbiano et al.
ISOTROPIC BUT MBH > 30 M (Pakull et al. 2002)
ANISOTROPIC BUT NOT BEAMED ( King et al 2001)
ANISOTROPIC & BEAMED (Mirabel & Rodriguez, 1999; Koerding & Falke 2002)
IMBHs DO NOT CONSTITUTE A LARGE FRACTION OF ULXs
VHE (>100 GeV) FROMRAY
BINARIES
LSI +61 303 with MAGIC
(Albert et al. Science 2006)
VHE emission is variable
LS 5039 with HESS
(Aharonian et al. Science 2005)
• Both have compact objects with masses M < 4 M
• Both are runaway HMXBs formed < 2 x 106 yrs ago
LS 5039 WAS EJECTED FROM THE GALACTIC PLANE
A VHE (> 100 GEV) SOURCEParedes, Ribo et al. 2002 Ribo, Paredes et al. 2002
V = 100-140 km/s; e~0.5; Mj = 2000-5000 Km/s M ; Mejected in SN = 5-15 M
LSI +61 303 WAS EJECTED FROM A CLUSTER
THE COMPACT OBJECT IN LSI +61 303 WAS FORMED < 2 Myr AGO IN AN ASYMMETRIC SN EXPOLSION
V ~ 27 km/s < 2 M were blown away
Linear momentum = 430 M km/s, as in runaway neutron stars
Mirabel, I. Rodrigues & Lu (A&A, 2004)
Massey et al. 1995
IC 1805
A VHE ( > 100 GEV) SOURCE
MODELS FOR -RAY BINARIES
1) IC of e- jets on UV photons (Paredes et al. 2002) or hadrons in the jets (Romero
et al. 2005) with matter of the stellar wind. Microblazars (Mirabel & Rodriguez,1999)
2) e- from pulsar wind on UV Photons (e.g. PSR B1259-63, Maraschi & Treves, 1981)
Mirabel (Science 309, 714, 2006)
VHE FROM COMPACT BINARIES• PULSAR WIND MODEL: Power by rotational energy (Dubus, 2006)
• PSR B1259-63, LS 5039 & LSI +61 303 have compact objects with M < 4 MSUN
• Time variability & x-ray spectrum of LSI +61 303 resemble those of young pulsars
• LSI +61 303 is a Be star like PSR B1259-63 & all known Be/X-ray binary are NSs
• But does not satisfactorily fit the GeV radio wavelength fluxes in LSI & LS 5039
• Definitive proof: Detection of pulsations in LS 5039 & LSI +61 303
• MICROQUASAR JET MODELS: Power by accretion (Bosch-Ramon)
• Particle energy in QSOs and QSOs are comparable (blazar-microblazar analogy)
• The kinetic power in QSOs is equal or larger than the radiated power
• Electrons in the jets are accelerated up to TeV energies
• LS 5039: jets are steady, two-sided, seem to have bulk motions of 0.2-0.3c as compact QSO jets, and no radio outbursts have been observed (Paredes et al.)
• Definitive proof: VHE emission from confirmed BHs (e.g Cyg X-1, V 4641,GRS 1915)
RADIO IMAGES WITH HIGHER SENSITIVITY AND RESOLUTION
GAMMA-RAY BURSTS OF LONG DURATION MARK
THE BIRTH OF BLACK HOLES AT COSMIC DISTANCES
• They are detected at large redshifts, up to z = 6.4
• They are exploding massive stars of low metallicity
• Associated with SN Ic & super-relativistic jets
QSO -QSO -GRB ANALOGYHAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, S&T 2002)
AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?
no
no ?
SUMMARYMicroquasars have provided insight into:
• THE PHYSICS OF RELATIVISTIC JETS FROM BH’s• THE CONNECTION BETWEEN ACCRETION & EJECTION
Microquasars could provide insight into:
• A LARGE FRACTION OF ULXs IN NEARBY GALAXIES
• GRBs OF LONG DURATION IN DISTANT GALAXIES
• THE PHYSICS IN THE JETS OF DISTANT BLAZARS
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 QSOs to find out:
•BIRTH PLACE & NATURE OF THE PROGENITOR STARS
•WHETHER THE PROGENITOR STAR ALWAYS EXPLODES AS AN ENERGETIC SUPERNOVAE
A BLACK HOLE IN THE GALACTIC HALO
XTE J1118+480 MBH~7 M M*=0.1–0.5 M ; l=158o b=+62o ; D=1.9 kpc
WAS THE BH FORMED IN THE HALO, THICK DISK OR IN
THE GALACTIC THIN DISK BY A VIOLENT NATAL KICK ?
GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs
Yellow: Sun White: BH binary
Orbit typical of globular clusters
(Mirabel, Dhawan et al Nature 2001)
but
Solar abundances in the star
imply that the black hole formed
in a SN that polluted the donnor
(astro-ph by Gonzalez et al. 2006)
A RUNAWAY BLACK HOLEA LIKELY FOSSIL OF A GRBs
FORMED IN AN HYPER-NOVA (Israelian et al. Nature 2001)
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
LOW-MASS BLACK HOLE FORMED
IN A LUMINOUS SUPERNOVA
GRO J1655-40 MBH ~ 4 M
ORBITS FOR THE LAST 230 Myrs
Yellow: Sun White: BH binary
THE GALACTIC TRIP OF SCORPIUS X-1
SCO X-1 FORMED IN A GLOBULAR CLUSTER OR GALACTIC BULGE
The best determined XRB path. Parallax and proper motion from Fomalont et al. (Mirabel & I. Rodrigues, 2003)
GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs
Yellow: Sun Red: BH binary
THE ~10 M BLACK HOLE IN
Cyg X-1 WAS BORN IN THE DARK
V < 9 +/- 2 km/s
< 1 M ejected in SN
Otherwise it would have been shot out from the parent association of massive stars
MASSIVE STELLAR BH FORM PROMPTLY
Mirabel & I. Rodrigues, Science (2003)
FORMATION OF THE BH IN GRS 1915+105
Moves in the Galactic plane with Vb = 0 +/- 4 km/sec
VBH = (33 to 70) +/- 12 km/s for D = 9 to 12 kpc (Chapuis & Corbel,2004)
But dispersion velocity of 6x109 yr old disk population is ~50 km/s
THE BH WAS FORMED PROMPTLY IN THE DISK
Black hole of 14 +/-4 M with a ~1 M donnor (Greiner et al. 2002-3) VLBA astrometry during 7 years: 6.8+/-0.2 mas/yr (Dhawan & M., 2005)
QPOs AND GENERAL RELATIVITYGRS 1915+105 (Strohmayer)
XTE & INDIAN SAT.
max = f(MBH, Spin) DETERMINE THE SPIN OF BLACK HOLES
THE BLACK HOLE SPIN & DISK TEMPERATURE SUGGEST
THAT JETS MAY BE POWERED BY THE BLACK HOLE SPIN
•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
Jerome Rodriguez et al.
SUMMARYMicroquasars 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
BLACK HOLE ASTROPHYSICS IS TODAY IN AN ANALOGOUS SITUATION AS WAS STELLAR ASTRONOMY IN THE FIRST HALF OF LAST CENTURY, WHEN THE HR DIAGRAM WAS CONSTRUCTED FOR FIRST TIME
IF THE EMPIRICAL CORRELATIONS
X-ray/radio/mass QPOs/mass Noise-spectrum/mass Gallo et al. 2004 Abramovics, 2005 Uttley et al. 2004
BECOME MORE ROBUST, INDEPENDENTLY OF THE MODELS, THE MASS AND SPIN OF BLACK HOLES WILL BE
DETERMINED
THE BLACK HOLE FUNDAMENTAL PLANE
Merloni et al. Falke, Koerding et al.
SUPERLUMINAL MOTIONS IN QSOs & AGN
•OBSERVED IN > 30 QSOs & AGN
•IN RADIO & OPTICAL WAVES
• PROPER MOTION SEEN IN YEARS
•Vapp UP TO 30c in blazars
•One sided because of Doppler boosting
•WHAT IS THE NATURE ?
“PLASMONS” OR SHOCKS ?