microquasars
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
MICROQUASARS
Felix Mirabel European Southern Observatory
Santiago, Chile
THE IDEA OF MICROQUASAR
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
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 ?
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
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
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
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
ANALOGOUS ACCRETION-JET CONNECTION IN THE SCALE-UPQSO3C 120 Marscher, Gomez, et al. Nature 2002
Red: X-rays
Yellow: Radio
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
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)
>50% OF THE RELEASED ENERGY IS NOT RADIATED
Cyg X-3 (Marti et al.2005)
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
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)
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
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
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
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
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)
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
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
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
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 ?
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 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
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
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
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