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MICROQUASARS. Five international workshops. Felix Mirabel European Southern Observatory. Chile. 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. - PowerPoint PPT Presentation
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MICROQUASARS
Felix Mirabel
European Southern Observatory. Chile
Five international workshops
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 & Luis 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) RELATIVISTIC ABERRATION IN ANTISYMMETRIC TWIN JETS
2) JETS ARE TWO-SIDED WHICH ALLOWS TO SOLVE EQUATIONS
3) MOVE ON THE PLANE OF THE SKY ~103 TIMES FASTER THAN AGN
4) AGN (e.g M87) BETTER TO COLLIMATION MECHANISM (Birreta, Livio…)
WITH SAME BULK LORENTZ FACTORS AS IN QSOsMirabel & Rodriguez, 1994
DARK JETS FROM BLACK HOLESSS433 Margon et al. (1979 - 1984)
Radio (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
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
ABSCENCE OF EVIDENCE FOR A MATERIAL SURFACE AROUND 14 Msun
THE ONSET OF THE JET IS AT THE TIME OF A X-RAY “SPIKE”:
SUDDEN REFILL OF THE DISK & SHOCK THROUGH COMPACT JET
T MBH Mirabel et al. (1998) 1 hr = 30 yr in SgrA*
COMPACT STEADY JETS
• ~100 AU IN LENGTH PRESENT DURING PLATEAU STATE
• SPEED OF THE FLOW < 0.4c (Ribo, Mirabel & Dhawan 2005)
• LARGE SCALE JETS ARE SHOCKS PROPAGATING c
THROUGH THE SLOWER MOVING COMPACT JET
• COMPACT JET USED TO MEASURE SPACE VELOCITIES
Ribo, Mirabel & Dhawan (2005) Mirabel et. al, 1998
2.0 cm 3.6 cm
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):
use the kinematics of QSOs to find out
•BIRTH PLACE & NATURE OF THE PROGENITOR STARS
•WHETHER THE PROGENITOR STAR ALWAYS EXPLODES AS AN ENERGETIC SUPERNOVA
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 THIS 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 & Rodrigues, 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 RUNAWAY HMXB LS 5039 A VHE (> 100 GEV) sources detected with HESS (Aharonian, Science 2005)
Paredes, Ribo et al. 2002 Ribo et al. 2002
V = 100-140 km/s; e~0.5; Mj = 2000-5000 Km/s M ; Mejected in SN = 5-15 M
MX ~3.7 Msolar Mdonor ~ 23 Msolar e = 0.35 Casares et al. (2005)
EJECTION OF A Be/XRB FROM A CLUSTER
V ~ 27 km/s < 2M were blown away. Linear momentum = 430 M km/s.
IF MASSIVE STAR FORMATION IN THE PARENT CLUSTERS IS COEVAL:
Low mass compact objects such as in LSI +61 303, the magnetar SGR 1806-20 (Fuchs et al. 1999) and a X-ray pulsar in Westerlund 1 (Muno et al. 2006) may have been formed from very massive progenitors (> 40 M )
Mirabel, I. Rodrigues & Lu (A&A, 2004)
Massey et al. 1995
IC 1805
LSI +61 303: a VHE (>100 GEV) source detected with MAGIC (Gonzalez et al. 2006)
THE GALACTIC TRIP OF SCORPIUS X-1
SCO X-1 FORMED IN A GLOBULAR CLUSTER OR GALACTIC BULGE
The best determined XRB path (Mirabel & I. Rodrigues, 2003)
GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs
Yellow: Sun Blue: 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)
By dynamic diffusion velocity of 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 donor (Greiner et al. 2002-3) VLBA astrometry during 7 yrs:6.8+/-0.2 mas/yr (Dhawan & Mirabel, 2005)
QSO -QSO -GRB ANALOGY HAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, Sky&Tel ( 2002)
AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?
neutron star
no
no ?
SUMMARYMicroquasars have provided insight into:
-THE PHYSICS OF RELATIVISTIC JETS FROM BH’s-THE CONNECTION BETWEEN ACCRETION & EJECTION-THE FORMATION OF BLACK HOLES AND NEUTRON STARS:
Can stars of >40 Msolar end as neutron stars rather than BHs ?
Do BHs of >10 Msolar form promptly rather than in bright SN ?
Microquasars could provide insight into:
• A LARGE FRACTION OF ULXs IN NEARBY GALAXIES
• GRBs OF LONG DURATION IN DISTANT GALAXIES