MICROQUASARS: DISK-JET COUPLING Felix Mirabel European Southern Observatory. Chile.
MICROQUASARS
description
Transcript of MICROQUASARS
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MICROQUASARS
Felix Mirabel European Southern Observatory
Santiago, Chile
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THE IDEA OF MICROQUASAR
Mirabel, Rodriguez, et al, 1992
Black Hole
Wang et al. ApJ 2002
Belanger, Goldwurm, Goldoni, ApJ 2003
INTEGRAL
Chandra
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QUASAR-MICROQUASAR ANALOGY
The scales of length and time are proportional to MBH
Rsh = 2GMBH/c2 ; T MBH
The maximum color temperatureof the accretion disk is:
Tcol M/ 10M)-1/4
(Shakura & Sunyaev, 1976)
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 1992, 94, 98
APPARENT SUPERLUMINAL MOTIONS IN QSOs AS IN QSOs ?
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SUPERLUMINAL EJECTION IN A QSO
1 arcsec
Mirabel & Rodriguez, 1994
Vapp = 1.3c for a DISTANCE = 12 Kpc
cm
THE PLASMA THAT RADIATES IN THE HARD
X-RAYS IS BLOWN IN SUPERLUMINAL JETS VLA
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SUPERLUMINAL MOTIONS IN AGN & QSOs
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)
WITH SAME BULK LORENTZ FACTORS Mirabel & Rodriguez, 1994
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ACCRETION–JET CONNECTION
• 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
T MBHMirabel et al. Nature 98; using RXTE + ESO + NRAO
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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
• THE COMPACT JET REAPPEARS HOURS AFTER FLARES
Ribo, Mirabel, Dhawan 2005 Mirabel et. al, 1998
2.0 cm 3.6 cm
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ANALOGOUS ACCRETION-JET CONNECTION IN THE SCALE-UPQSO3C 120 Marscher, Gomez, et al. Nature 2002
Red: X-rays
Yellow: Radio
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DARK JETS FROM BLACK HOLES
(Dubner et al) X-rays: (Brinkmann et al)
SS433/W50
• ATOMIC NUCLEI MOVING AT 0.26c
• MECHANICAL LUMINOSITY > 1040 erg/sec
• NON RADIATIVE JETS = “DARK” JETS
1o = 60 pcarcsec
VLA 20cm
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LARGE-SCALE JETS IN GRS 1915+105(TRIGGERING STAR FORMATION ?)
Rodriguez & Mirabel, 2000
Variable NT feature ?
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OTHER LARGE-SCALE JETS ?Cyg X-1 ( Gallo et al. Nature 2005)
>50% OF THE RELEASED ENERGY IS NOT RADIATED
Cyg X-3 (Marti et al.2005)
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MOVING X-RAY JETS IN A QSOQSOs XTE J1550-564 & Corbel et al. (2002, 05)
X-rays are produced by synchrotron electrons accelerated to TeV energies
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MICROBLAZARS (Mirabel. & Rodriguez, ARAA 1999)
Due to relativistic beaming: t
e.g. If = 5, t < 1/50 and I > 103
SHOULD APPEAR AS SOURCES WITH FAST
AND INTENSE VARIATIONS OF FLUX
DIFFICULT TO FOLLOW AND TO FIND
blazars 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)
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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
around compact objects of < 4
•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)
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
LS 5039
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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
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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 QSOs ARE FOSSILS OF GRBs
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RUNAWAY BLACK HOLEMirabel, 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
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
GRO J1655-40 MBH ~ 4 M
ORBITS FOR THE LAST 230 Myrs
Yellow: Sun White: BH binary
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THE HIGH MASS BLACK HOLE IN Cyg X-1 FORMED IN THE DARK
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 ?
Mirabel & Rodrigues, Science (2003)
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A BLACK HOLE FORMED ~7 BILLONS YEARS AGO IN THE GALACTIC HALO
Mirabel, Rodrigues et al.
Nature, 2001
XTE J1118+480MBH = 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
GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs
Yellow: Sun White: BH binary
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THE QSO/AGN ANALOGY IS CONFIRMED AND MAY BE USED TO GAIN KNOWLEDGE IF THE PHENOMENOLOGICAL CORRELATIONS QSO/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
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Fe K LINES IN QSOsCygnus X-1 Miller et al. (2002)
CHANDRA, XMM & Beppo-SAX
•Asymmetry: gravitational redshift,
Doppler & transverse-Doppler shift
•Narrow component from outer disk ?
•Broad component from inner disk
SPINNING BLACK HOLE?
QSOs MAY BE GOOD LABORATORIES TO STUDY IN SHORT TIME SCALES THE Fe KLINES AS A FUNCTION OF X-RAY STATE
TO TEST MODELS ON THE ORIGIN OF THESE LINES IN SEYFERTS
FOUND IN ~6 MICROQASARS
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QSO -QSO -GRB ANALOGYHAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, S&T 2002)
AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?
neutron star
no
no ?
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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
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X-RAY - RADIO CORRELATIONS IN LOW-POWER BHs OF ALL MASSES
Radio-X-ray correlation in low-hard state QSOs
(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
QSOs 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
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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 QSOs and the spin of s
In 3 QSOs 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). T ratio ~ MSgrA BH / Mstellar BH = 105-6
Independently of the model
The BH mass in ULXs may be derived
Strohmayer
GRS 1915+105
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APERIODIC VARIABILITY IN AGN & QSOs
• 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
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QPOs AND GENERAL RELATIVITYGRS 1915+105 (Strohmayer)
XTE & INDIAN SAT.
max = 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)
•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
Tagger; Chakrabarti, Zhang