MICROQUASARS

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