Transcript MICROQUASARS - Osservatorio Astronomico di Roma-INAF

MICROQUASARS
Felix Mirabel
European Southern Observatory
Santiago, Chile
THE IDEA OF MICROQUASAR
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 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 ?
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
Vapp = 1.3c
for a
DISTANCE = 12 Kpc
VLA
SUPERLUMINAL MOTIONS IN AGN & mQSOs
Mirabel & Rodriguez, 1994
WITH SAME BULK LORENTZ FACTORS
1) MOVE ON THE PLANE OF THE SKY ~103 TIMES FASTER
2) JETS ARE TWO-SIDED WHICH ALLOWS TO SOLVE EQUATIONS
3) BETTER AGN AT <100 Mpc. e.g. Collimation @ 30-100 Rsh in M87 (Biretta)
ACCRETION–JET 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
COMPACT STEADY JETS
Ribo, Mirabel, Dhawan 2005
2.0 cm
Mirabel et. al, 1998
3.6 cm
• ~100 AU IN LENGTH PRESENT DURING PLATEAU STATE
• SPEED OF THE FLOW < 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
ANALOGOUS ACCRETION-JET CONNECTION IN THE
SCALE-UP mQSO 3C 120
Red:
X-rays
Yellow: Radio
Marscher, Gomez, et al. Nature 2002
DARK JETS FROM BLACK HOLES
(Dubner et al) X-rays: (Brinkmann et al)
VLA l20cm
SS433/W50
1arcsec
1o = 60 pc
• ATOMIC NUCLEI MOVING AT 0.26c 
• MECHANICAL LUMINOSITY > 1040 erg/sec
• NON RADIATIVE JETS = “DARK” JETS
LARGE-SCALE JETS IN GRS 1915+105
(TRIGGERING STAR FORMATION ?)
Rodriguez & Mirabel, 2000
Variable NT feature ?
OTHER LARGE-SCALE JETS ?
Cyg X-1
( Gallo et al. Nature 2005)
Cyg X-3 (Marti et al.2005)
>50% OF THE RELEASED ENERGY IS NOT RADIATED
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
MICROBLAZARS
(Mirabel. & Rodriguez, ARAA 1999)
Due to relativistic beaming: Dt a 1/2g2 ; 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
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)
HAVE TWO MICROBLAZARS BEEN FOUND ?
Paredes et al. 2004
LS 5039
•Both inside EGRET error box (MeV-GeV)
•LS 5039 has HESS counterpart >100 GeV
(Aharonian et al. Science 2005)
•Both are massive stars in eccentric orbits
LS 5039
LSI +61 303 Massi et al.04
around compact objects of < 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)
Alternative model: Relativistic wind from young pulsar
e.g.: PSR B1259-63 in HMXB detected by HESS at periastron
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
GAMMA-RAY BURSTS OF LONG DURATION MARK THE
BIRTH OF BLACK HOLES AT COSMIC DISTANCES
Association with JETS, SN Ic & GRB @ Z=6.4 
PROGENITORS OF GRB’s ARE MASSIVE BINARIES
 SOME mQSOs ARE FOSSILS OF GRBs
RUNAWAY BLACK HOLE
Mirabel, Irapuan Rodrigues et al.
GRO J1655-40
MBH ~ 4 M
ORBITS FOR THE LAST 230 Myrs
Yellow: Sun
White: BH binary
(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
A LIKELY FOSSIL OF A GRBs
FORMED IN AN HYPER-NOVA
(Israelian et al. Nature 2001)
LOW-MASS BLACK HOLE FORMED
IN A LUMINOUS SUPERNOVA
THE HIGH MASS BLACK HOLE
IN Cyg X-1 FORMED IN THE DARK
Mirabel & Rodrigues, Science (2003)
V < 9 +/- 2 km/s

< 1 M ejected in SN
Otherwise it would
have shot out from
the parent association
MBH > 10 M
MASSIVE STELLAR BH’s FORM PROMPTLY ?
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 J1118+480
MBH = 9 M
l=158o b=+62o; D=1.9 kpc
GALACTIC ARCHEOLOGY
OF MASSIVE STARS
PROBABLY ONE OF THE SEVERAL MILLONS BHs
THAT ESCAPED FROM GLOBULAR CLUSTERS
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
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
QSO - mQSO - GRB ANALOGY
HAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, S&T 2002)
neutron star
no
?
no
AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?
CONCLUSION
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
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
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) 3:2 twin peak kHz QPO in mQSOs and the spin of BHs
Strohmayer
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).
DT ratio ~ MSgrA BH / Mstellar BH = 105-6
Independently of the model
The BH mass in ULXs may be derived
GRS 1915+105
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
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.) 
Tagger; Chakrabarti, Zhang
must depend on fundamental properties of black hole
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)