Download MICROQUASARS

MICROQUASARS
Five international workshops
VI in Como, Italy (18-22 Sept. 2006)
Felix Mirabel
European Southern Observatory. Chile
on leave from CEA-Saclay. France
HIGH ENERGY SOURCES IN THE GALACTIC CENTRE
Mirabel, Rodriguez, et al, 1992
Wang et al. ApJ 2002
Chandra
Belanger, Goldwurm, Goldoni, ApJ 2003
INTEGRAL
Black Hole
QUASAR-MICROQUASAR ANALOGY
QUASAR
MICROQUASAR
Mirabel & Rodriguez (Nature 1998)
The scales of length and time
are proportional to MBH
Rsh = 2GMBH/c2 ; DT a MBH
Unique system of equations:
The maximum color temperature
of the accretion disk is:
Tcol a (M/ 10M)-1/4
(Shakura & Sunyaev, 1976)
Waited era of space astronomy
For a given accretion rate:
LBol a MBH ; ljet a MBH ;
j a MBH-1 ; B a MBH-1/2
(Sams, Eckart, Sunyaev, 96; Rees 04)
APPARENT SUPERLUMINAL MOTIONS IN mQSOs AS IN QSOs ?
SUPERLUMINAL EJECTION IN A mQSO
Mirabel & Rodriguez, 1994
THE PLASMA THAT RADIATES IN THE HARD
X-RAYS IS BLOWN IN SUPERLUMINAL JETS
l3.6 cm
1 arcsec
GRS 1915+105
Vapp > C
for a
DISTANCE > 8 Kpc
VLA
SUPERLUMINAL MOTIONS IN THE GALAXY
1) ASYMMETRIES DUE TO RELATIVISTIC ABERRATION IN TWIN JETS
2) mQSOs 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 HOLES
Radio (Dubner et al); X-rays: (Brinkmann et al)
VLA l20cm
SS433/W50
1arcsec
1o = 60 pc
• ATOMIC NUCLEI MOVING AT 0.26c 
• MECHANICAL LUMINOSITY > 1039 erg/sec
• NON RADIATIVE JETS = “DARK” JETS
• >50% OF THE ENERGY IS NOT RADIATED
LARGE-SCALE JETS IN CYGNUS X-1
Gallo, Fender et al. Nature 2005
ring diameter = 5 pc
> 50% OF THE RELEASED
ENERGY IS NOT RADIATED
IS IT A VHE SOURCE ?
LARGE-SCALE JETS
IN GRS 1915+105 ?
Rodriguez & Mirabel (2006)
hot spots at ~ 50 pc
MOVING X-RAY JETS IN A mQSO
mQSOs XTE J1550-564 & H1743-322
Corbel et al. Science 2002, 05
X-rays are produced by synchrotron  electrons accelerated to TeV energies
ACCRETION–JET CONNECTION
DT a MBH
1 hr = 30 yr in SgrA*
Mirabel, Dhawan, Rodriguez (1998)
GRS 1915+105
- 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
-
COMPACT STEADY JETS
Ribo, Dhawan & Mirabel (2005)
2.0 cm
GRS 1915+105
Mirabel, Dhawan, et al. 1998
3.6 cm
• ~100 AU IN LENGTH PRESENT DURING PLATEAU STATE
• SPEED OF THE FLOW < 0.4c (Ribo, Dhawan & Mirabel 2005)
• LARGE SCALE JETS ARE SHOCKS PROPAGATING AT ~0.98c
THROUGH THE SLOWER MOVING COMPACT JET
mQSOs & ULTRALUMINOUS X-RAY SOURCES
Microquasars in external galaxies
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
Fabbiano et al.
X-ray (Chandra)
Antennae
VHE (>100 GeV) FROM g-RAY BINARIES
LS 5039 with HESS
LSI +61 303 with MAGIC
(Aharonian et al. Science 2005)
(Albert et al. Science 2006)
VHE emission is variable
• 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) SOURCE
Paredes, 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
A VHE ( > 100 GEV) SOURCE
Mirabel, I. Rodrigues & Lu (A&A, 2004)
Massey et al. 1995
IC 1805
V ~ 27 km/s  < 2 M were blown away
Linear momentum = 430 M km/s, as in runaway neutron stars
THE COMPACT OBJECT IN LSI +61 303 WAS FORMED
< 2 Myr AGO IN AN ASYMMETRIC SN EXPOLSION
MODELS FOR g-RAY BINARIES
Mirabel (Science 309, 714, 2006)
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)
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 mQSOs are comparable (blazar-microblazar analogy)
The kinetic power in mQSOs 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 mQSO 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 - mQSO - GRB ANALOGY
HAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, S&T 2002)
no
?
no
AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?
SUMMARY
Microquasars 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 mQSOs 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
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)
WAS THE BH FORMED IN THE HALO, THICK DISK OR IN
THE GALACTIC THIN DISK BY A VIOLENT NATAL KICK ?
A RUNAWAY BLACK HOLE
GRO J1655-40
MBH ~ 4 M
ORBITS FOR THE LAST 230 Myrs
Yellow: Sun
A LIKELY FOSSIL OF A GRBs
FORMED IN AN HYPER-NOVA
(Israelian et al. Nature 2001)
White: BH binary
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
THE GALACTIC TRIP OF SCORPIUS X-1
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
SCO X-1 FORMED IN A GLOBULAR CLUSTER OR GALACTIC BULGE
THE ~10 M BLACK HOLE IN
Cyg X-1 WAS BORN IN THE DARK
Mirabel & I. Rodrigues, Science (2003)
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
FORMATION OF THE BH IN GRS 1915+105
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)
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
QPOs AND GENERAL RELATIVITY
XTE & INDIAN SAT.
GRS 1915+105 (Strohmayer)
•High frequency QPOs (e.g. 40 & 67 Hz repeat in GRS)
•This 3:2 ratio now found in 4 BHXBs (Remillard et al.) 
Jerome Rodriguez et al.
must depend on fundamental properties of black hole
nmax = 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
SUMMARY
Microquasars 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
Gallo et al. 2004
QPOs/mass
Abramovics, 2005
Noise-spectrum/mass
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 ?