MICROQUASARS

1
MICROQUASARS
Felix Mirabel European Southern
Observatory Santiago, Chile
2
THE IDEA OF MICROQUASAR

Mirabel, Rodriguez, et al, 1992
Wang et al. ApJ 2002
Chandra
Belanger, Goldwurm, Goldoni, ApJ 2003
INTEGRAL

Black Hole
3
QUASAR-MICROQUASAR ANALOGY


QUASAR MICROQUASAR
Mirabel Rodriguez Nature 1992, 94, 98

• The scales of length and time are proportional to
  MBH
• Rsh 2GMBH/c2 DT a MBH
• The maximum color temperature
• of the accretion disk is
• Tcol a (M/ 10M?)-1/4
• (Shakura Sunyaev, 1976)
• 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
?
4
SUPERLUMINAL EJECTION IN A mQSO
Mirabel Rodriguez, 1994
THE PLASMA THAT RADIATES IN THE HARD X-RAYS IS
BLOWN IN SUPERLUMINAL JETS
VLA
1 arcsec
l3.6 cm
Vapp 1.3c for a DISTANCE 12 Kpc
5
SUPERLUMINAL MOTIONS IN AGN mQSOs

WITH SAME BULK LORENTZ FACTORS
Mirabel Rodriguez, 1994

• MOVE ON THE PLANE OF THE SKY 103 TIMES FASTER
• JETS ARE TWO-SIDED WHICH ALLOWS TO SOLVE
  EQUATIONS
• BETTER AGN AT lt100 Mpc. e.g. Collimation _at_ 30-100
  Rsh in M87 (Biretta)

6
ACCRETIONJET CONNECTION
DT a MBH
Mirabel et al. Nature 98 using RXTE ESO NRAO

• INFRARED RADIO SYNCHROTRON EMISSION FROM THE
  JETS
• JETS APPEAR 5 MIN AFTER DISAPPEARANCE OF THE
  INNER DISK
• THE ONSET OF THE JET IS AT THE TIME OF A SPIKE
  IN THE X-RAYS SUDDEN REBUILT OF THE INNER
  DISK LAUNCH A SHOCK THROUGH

7
COMPACT STEADY JETS
Ribo, Mirabel, Dhawan 2005
Mirabel et. al, 1998
2.0 cm 3.6 cm

• 100 AU IN LENGTH PRESENT DURING PLATEAU STATE
• SPEED OF THE FLOW lt 0.4c (Ribo, Mirabel Dhawan
  2005)
• LARGE SCALE JETS ARE SHOCKS PROPAGATING AT
  0.98c
• THROUGH THE SLOWER MOVING COMPACT JET
• THE COMPACT JET REAPPEARS HOURS AFTER FLARES

8
ANALOGOUS ACCRETION-JET CONNECTION IN THE
SCALE-UP mQSO 3C 120 Marscher, Gomez, et
al. Nature 2002
Red X-rays Yellow Radio
9
DARK JETS FROM BLACK HOLES
(Dubner et al) X-rays (Brinkmann et al)
SS433/W50
VLA l20cm
1o 60 pc
1arcsec

• ATOMIC NUCLEI MOVING AT 0.26c ?
• MECHANICAL LUMINOSITY gt 1040 erg/sec
• NON RADIATIVE JETS DARK JETS

10
LARGE-SCALE JETS IN GRS 1915105(TRIGGERING STAR
FORMATION ?)
Rodriguez Mirabel, 2000
Variable NT feature ?
11
OTHER LARGE-SCALE JETS ?
Cyg X-1 ( Gallo et al. Nature 2005)
Cyg X-3 (Marti et al.2005)
gt50 OF THE RELEASED ENERGY IS NOT RADIATED
12
MOVING X-RAY JETS IN A mQSO
mQSOs XTE J1550-564 H1743-322
Corbel et al. (2002, 05)
X-rays are produced by synchrotron ? electrons
accelerated to TeV energies
13
MICROBLAZARS (Mirabel. Rodriguez, ARAA 1999)

• Due to relativistic beaming Dt a 1/2g2
  I a 8g3
• e.g. If g 5, Q lt 10o ? Dt lt 1/50 and
  DI gt 103
• SHOULD APPEAR AS SOURCES WITH FAST
• AND INTENSE VARIATIONS OF FLUX ?
• DIFFICULT TO FOLLOW AND TO FIND
• mblazars from HMXBs may appear as variable
  gamma-ray
• sources due to Inverse Compton on UV photons of
  donor
• (Romero, Kauffman, Mirabel 2002
  Bosch-Ramon Paredes, 2004)

14
HAVE TWO MICROBLAZARS BEEN FOUND ?
Paredes et al. 2004

• Both inside EGRET error box (MeV-GeV)
• LS 5039 has HESS counterpart gt100 GeV
• (Aharonian et al. Science
  2005)
• Both are massive stars in eccentric orbits
• around compact objects of lt 4 M?
• Both are young runaway compact binaries
• (Ribo et al. 2002 Mirabel Rodrigues
  2004)
• X-ray time variability supports scenario of
• jets fed by disks (Massi Bosch-Ramon et al.
  2005)

LS 5039
LS 5039
LSI 61 303 Massi et al.04
Alternative model Relativistic wind from young
pulsar e.g. PSR B1259-63 in HMXB detected by
HESS at periastron
15
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

16
GAMMA-RAY BURSTS OF LONG DURATION MARK THE BIRTH
OF BLACK HOLES AT COSMIC DISTANCES
Association with JETS, SN Ic GRB _at_ Z6.4 ?
PROGENITORS OF GRBs ARE MASSIVE BINARIES ?
SOME mQSOs ARE FOSSILS OF GRBs

17
RUNAWAY BLACK HOLE
Mirabel, Irapuan Rodrigues et al. (AA 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 A LIKELY FOSSIL OF A GRBs FORMED
IN AN HYPER-NOVA (Israelian et al. Nature 2001)
GRO J1655-40 MBH 4 M?
ORBITS FOR THE LAST 230 Myrs Yellow Sun
White BH binary
LOW-MASS BLACK HOLE FORMED IN A LUMINOUS
SUPERNOVA
18
THE HIGH MASS BLACK HOLE IN Cyg X-1 FORMED IN
THE DARK
Mirabel Rodrigues, Science (2003)
V lt 9 /- 2 km/s ? lt 1 M? ejected in
SN Otherwise it would have shot out from
the parent association MBH gt 10 M?
MASSIVE STELLAR BHs FORM PROMPTLY ?
19
A BLACK HOLE FORMED 7 BILLONS YEARS AGO IN THE
GALACTIC HALO
GALACTOCENTRIC ORBIT FOR THE LAST 230
Myrs Yellow Sun White BH binary
Mirabel, Rodrigues et al. Nature, 2001 XTE
J1118480 MBH 9 M? l158o b62o D1.9
kpc GALACTIC ARCHEOLOGY OF MASSIVE STARS

PROBABLY ONE OF THE SEVERAL MILLONS BHs THAT
ESCAPED FROM GLOBULAR CLUSTERS
20

• THE mQSO/AGN ANALOGY IS CONFIRMED AND MAY BE
  USED TO GAIN KNOWLEDGE
• IF THE PHENOMENOLOGICAL CORRELATIONS
  mQSO/AGN
• 1) X-ray/radio/mass, 2) QPOs/mass, 3)
  Noise-spectrum/mass
• became robust, independently of
  the models
• ESTIMATE THE MASS OF BLACK HOLES
• ANALOGOUS SITUATION OF H-R DIAGRAM IN STELLAR
  ASTRONOMY

21
Fe Ka LINES IN mQSOs
Cygnus X-1 Miller et al. (2002)
FOUND IN 6 MICROQASARS

• CHANDRA, XMM Beppo-SAX
• Asymmetry gravitational redshift,
• Doppler transverse-Doppler shift
• Narrow component from outer disk ?
• Broad component from inner disk
• SPINNING BLACK HOLE?

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
22
QSO - mQSO - GRB ANALOGY
HAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel
Rodriguez, ST 2002)

neutron star
no ?
no
AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR
JETS ?
23
CONCLUSION Microquasars have provided insight
into

• THE PHYSICS OF RELATIVISTIC JETS FROM BHs
• 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

24
X-RAY - RADIO CORRELATIONS IN LOW-POWER BHs OF
ALL MASSES
Radio-X-ray correlation in low-hard state
mQSOs (Corbel et al. 02 Gallo, Fender Pooley,
03 Maccarone et al.03) The power output of
quiescent BHs is jet-dominated In high-soft X-ray
state the radio jets are quenched. Also in AGN.
Sgr A, LINERs, FR I BL Lac are analogous to
mQSOs in the low-hard state (Falcke,et al.
04)
Relation between X-ray, radio mass of BHs
5 GHz 2-10 keV core emission (Merloni, Heinz
Di Matteo 03) From radiativelly inefficient
accretion rather than thin synchrotron
Radio/bolometric luminosity larger in AGN (Heinz
Sunyaev 2003) If more robust, independently
of the model
THE MASS OF BLACK HOLES COULD BE INFERRED
25
TIME VARIATIONS SEEM TO SCALE WITH BLACK HOLE
MASS
1) Duration of X-ray flares in Cyg X-1 and Sgr A
In Cyg X-1 and other BHXRBs 1-10 ms (Gierlinski
Zdziarski, 03) In Sgr A 400-10,000 s
(Baganoff et al. 01 Goldwurm et al. 03) 2) 32
twin peak kHz QPO in mQSOs and the spin of BHs In
3 mQSOs a J/(GM/c2) 0.6-0.9 (Remillard
2004) Due to gravitational cyclic modes
(Abramowicz et al. 2004)
Observations in Sgr A
IR QPOs of 17 min ? a 0.52
(Genzel et al. Nature. 04) X-ray QPOs that
include twins of 12 19 min (Aschenbach et al.
04).
Strohmayer
GRS 1915105
DT ratio MSgrA BH / Mstellar BH 105-6
Independently of the model The BH mass in
ULXs may be derived
26
APERIODIC VARIABILITY IN AGN mQSOs

• The break time scale in the power spectral
  density of black holes seems to scale linearly
  with the mass of the BH (Uttley McHardy, 2001)
• The NLS1 NGC 4051 scales better with Cyg X-1 in
  the soft-high state (Lbol 0.3 Ledd)
• The broad band Sey 1 NGC 3516 scales linearly
• with Cyg X-1 in the low-hard state
  (McHardy, 04)
• Most of the aperiodic variation in Cyg X-1 is due
  to the harder component (Churazov, Gilfanov,
  Revnivtsev, 2001)
• Propagating perturbations in the accreting flow
  (Uttley, 2004)

THE MASS OF BLACK HOLES IN ULXs COULD BE
DETERMINED
27
QPOs AND GENERAL RELATIVITY

GRS 1915105 (Strohmayer)

• High frequency QPOs (e.g. 40 67 Hz repeat in
  GRS)
• This 32 ratio now found in 4 BHXBs (Remillard et
  al.) ?
• must depend on fundamental properties of black
  hole

Tagger Chakrabarti, Zhang
nmax f(MBH, Spin) ? DETERMINE THE SPIN OF
BLACK HOLES THE BH SPIN DISK TEMPERATURE
SUGGEST THAT JETS MAY BE POWERED BY THE
BH SPIN (Zhang et al. Wang)