MICROQUASARS

Felix Mirabel

European Southern Observatory. Chile

on leave from CEA-Saclay. France

Five international workshops

VI in Como, Italy (18-22 Sept. 2006)

HIGH ENERGY SOURCES IN THE GALACTIC CENTRE

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

Unique system of equations: The maximum color temperatureof the accretion disk is:

Tcol M/ 10M)-1/4

(Shakura & Sunyaev, 1976)Waited era of space astronomy

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 1998)

APPARENT SUPERLUMINAL MOTIONS IN QSOs AS IN QSOs ?

SUPERLUMINAL EJECTION IN A QSO

1 arcsec

Mirabel & Rodriguez, 1994

Vapp > C for a DISTANCE > 8 Kpc

cm

THE PLASMA THAT RADIATES IN THE HARD

X-RAYS IS BLOWN IN SUPERLUMINAL JETS VLA

GRS 1915+105

SUPERLUMINAL MOTIONS IN THE GALAXY

1) ASYMMETRIES DUE TO RELATIVISTIC ABERRATION IN TWIN JETS

2) QSOs HAVE SAME BULK LORENTZ FACTORS AS QSOs & BLAZARS

3) JET COLLIMATION @ 30-100 Rsh IN M87 IS CONSISTENT WITH THE

BLANDFORD-PAYNE MODEL (Biretta et al., 2004). HADRONIC JETS ?

DARK JETS FROM BLACK HOLESRadio (Dubner et al); X-rays: (Brinkmann et al)

SS433/W50

• ATOMIC NUCLEI MOVING AT 0.26c

• MECHANICAL LUMINOSITY > 1039 erg/sec

• NON RADIATIVE JETS = “DARK” JETS

• >50% OF THE ENERGY IS NOT RADIATED

1o = 60 pcarcsec

VLA 20cm

LARGE-SCALE JETS IN CYGNUS X-1

Gallo, Fender et al. Nature 2005

ring diameter = 5 pc

LARGE-SCALE JETS IN GRS 1915+105 ? Rodriguez & Mirabel (2006)

hot spots at ~ 50 pc

> 50% OF THE RELEASED

ENERGY IS NOT RADIATED

IS IT A VHE SOURCE ?

MOVING X-RAY JETS IN A QSOQSOs XTE J1550-564 & Corbel et al. Science 2002, 05

X-rays are produced by synchrotron electrons accelerated to TeV energies

ACCRETION–JET CONNECTION

- THE ONSET OF THE JET IS AT THE TIME OF A X-RAY “SPIKE” - SUDDEN REFILL OF THE INNER DISK & INJECTION INTO THE JETS - SHOCK THROUGH A MILDLY RELATIVISTIC COMPACT JET

T MBH Mirabel, Dhawan, Rodriguez (1998) 1 hr = 30 yr in SgrA*

GRS 1915+105

COMPACT STEADY JETS

• ~100 AU IN LENGTH PRESENT DURING PLATEAU STATE

• SPEED OF THE FLOW < 0.4c (Ribo, Dhawan & Mirabel 2005)

• LARGE SCALE JETS ARE SHOCKS PROPAGATING c

THROUGH THE SLOWER MOVING COMPACT JET

Ribo, Dhawan & Mirabel (2005) Mirabel, Dhawan, et al. 1998

2.0 cm 3.6 cm

GRS 1915+105

QSOs & ULTRALUMINOUS X-RAY SOURCES Microquasars in external galaxies

X-ray (Chandra) AntennaeFabbiano et al.

ISOTROPIC BUT MBH > 30 M (Pakull et al. 2002)

ANISOTROPIC BUT NOT BEAMED ( King et al 2001)

ANISOTROPIC & BEAMED (Mirabel & Rodriguez, 1999; Koerding & Falke 2002)

IMBHs DO NOT CONSTITUTE A LARGE FRACTION OF ULXs

VHE (>100 GeV) FROMRAY

BINARIES

LSI +61 303 with MAGIC

(Albert et al. Science 2006)

VHE emission is variable

LS 5039 with HESS

(Aharonian et al. Science 2005)

• Both have compact objects with masses M < 4 M

• Both are runaway HMXBs formed < 2 x 106 yrs ago

LS 5039 WAS EJECTED FROM THE GALACTIC PLANE

A VHE (> 100 GEV) SOURCEParedes, Ribo et al. 2002 Ribo, Paredes et al. 2002

V = 100-140 km/s; e~0.5; Mj = 2000-5000 Km/s M ; Mejected in SN = 5-15 M

LSI +61 303 WAS EJECTED FROM A CLUSTER

THE COMPACT OBJECT IN LSI +61 303 WAS FORMED < 2 Myr AGO IN AN ASYMMETRIC SN EXPOLSION

V ~ 27 km/s < 2 M were blown away

Linear momentum = 430 M km/s, as in runaway neutron stars

Mirabel, I. Rodrigues & Lu (A&A, 2004)

Massey et al. 1995

IC 1805

A VHE ( > 100 GEV) SOURCE

MODELS FOR -RAY BINARIES

1) IC of e- jets on UV photons (Paredes et al. 2002) or hadrons in the jets (Romero

et al. 2005) with matter of the stellar wind. Microblazars (Mirabel & Rodriguez,1999)

2) e- from pulsar wind on UV Photons (e.g. PSR B1259-63, Maraschi & Treves, 1981)

Mirabel (Science 309, 714, 2006)

VHE FROM COMPACT BINARIES• PULSAR WIND MODEL: Power by rotational energy (Dubus, 2006)

• PSR B1259-63, LS 5039 & LSI +61 303 have compact objects with M < 4 MSUN

• Time variability & x-ray spectrum of LSI +61 303 resemble those of young pulsars

• LSI +61 303 is a Be star like PSR B1259-63 & all known Be/X-ray binary are NSs

• But does not satisfactorily fit the GeV radio wavelength fluxes in LSI & LS 5039

• Definitive proof: Detection of pulsations in LS 5039 & LSI +61 303

• MICROQUASAR JET MODELS: Power by accretion (Bosch-Ramon)

• Particle energy in QSOs and QSOs are comparable (blazar-microblazar analogy)

• The kinetic power in QSOs is equal or larger than the radiated power

• Electrons in the jets are accelerated up to TeV energies

• LS 5039: jets are steady, two-sided, seem to have bulk motions of 0.2-0.3c as compact QSO jets, and no radio outbursts have been observed (Paredes et al.)

• Definitive proof: VHE emission from confirmed BHs (e.g Cyg X-1, V 4641,GRS 1915)

RADIO IMAGES WITH HIGHER SENSITIVITY AND RESOLUTION

GAMMA-RAY BURSTS OF LONG DURATION MARK

THE BIRTH OF BLACK HOLES AT COSMIC DISTANCES

• They are detected at large redshifts, up to z = 6.4

• They are exploding massive stars of low metallicity

• Associated with SN Ic & super-relativistic jets

QSO -QSO -GRB ANALOGYHAVE THE SAME 3 BASIC INGREEDIENTS (Mirabel & Rodriguez, S&T 2002)

AN UNIVERSAL MAGNETO-HYDRODINAMIC MECHANISM FOR JETS ?

no

no ?

SUMMARYMicroquasars have provided insight into:

• THE PHYSICS OF RELATIVISTIC JETS FROM BH’s• THE CONNECTION BETWEEN ACCRETION & EJECTION

Microquasars could provide insight into:

• A LARGE FRACTION OF ULXs IN NEARBY GALAXIES

• GRBs OF LONG DURATION IN DISTANT GALAXIES

• THE PHYSICS IN THE JETS OF DISTANT BLAZARS

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

A BLACK HOLE IN THE GALACTIC HALO

XTE J1118+480 MBH~7 M M*=0.1–0.5 M ; l=158o b=+62o ; D=1.9 kpc

WAS THE BH FORMED IN THE HALO, THICK DISK OR IN

THE GALACTIC THIN DISK BY A VIOLENT NATAL KICK ?

GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs

Yellow: Sun White: BH binary

Orbit typical of globular clusters

(Mirabel, Dhawan et al Nature 2001)

but

Solar abundances in the star

imply that the black hole formed

in a SN that polluted the donnor

(astro-ph by Gonzalez et al. 2006)

A RUNAWAY BLACK HOLEA LIKELY FOSSIL OF A GRBs

FORMED IN AN HYPER-NOVA (Israelian et al. Nature 2001)

Mirabel, 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

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 GALACTIC TRIP OF SCORPIUS X-1

SCO X-1 FORMED IN A GLOBULAR CLUSTER OR GALACTIC BULGE

The best determined XRB path. Parallax and proper motion from Fomalont et al. (Mirabel & I. Rodrigues, 2003)

GALACTOCENTRIC ORBIT FOR THE LAST 230 Myrs

Yellow: Sun Red: BH binary

THE ~10 M BLACK HOLE IN

Cyg X-1 WAS BORN IN THE DARK

V < 9 +/- 2 km/s

< 1 M ejected in SN

Otherwise it would have been shot out from the parent association of massive stars

MASSIVE STELLAR BH FORM PROMPTLY

Mirabel & I. Rodrigues, Science (2003)

FORMATION OF THE BH IN GRS 1915+105

Moves in the Galactic plane with Vb = 0 +/- 4 km/sec

VBH = (33 to 70) +/- 12 km/s for D = 9 to 12 kpc (Chapuis & Corbel,2004)

But dispersion velocity of 6x109 yr old disk population is ~50 km/s

THE BH WAS FORMED PROMPTLY IN THE DISK

Black hole of 14 +/-4 M with a ~1 M donnor (Greiner et al. 2002-3) VLBA astrometry during 7 years: 6.8+/-0.2 mas/yr (Dhawan & M., 2005)

QPOs AND GENERAL RELATIVITYGRS 1915+105 (Strohmayer)

XTE & INDIAN SAT.

max = f(MBH, Spin) DETERMINE THE SPIN OF BLACK HOLES

THE BLACK HOLE SPIN & DISK TEMPERATURE SUGGEST

THAT JETS MAY BE POWERED BY THE BLACK HOLE SPIN

•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

Jerome Rodriguez et al.

SUMMARYMicroquasars 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

BLACK HOLE ASTROPHYSICS IS TODAY IN AN ANALOGOUS SITUATION AS WAS STELLAR ASTRONOMY IN THE FIRST HALF OF LAST CENTURY, WHEN THE HR DIAGRAM WAS CONSTRUCTED FOR FIRST TIME

IF THE EMPIRICAL CORRELATIONS

X-ray/radio/mass QPOs/mass Noise-spectrum/mass Gallo et al. 2004 Abramovics, 2005 Uttley et al. 2004

BECOME MORE ROBUST, INDEPENDENTLY OF THE MODELS, THE MASS AND SPIN OF BLACK HOLES WILL BE

DETERMINED

THE BLACK HOLE FUNDAMENTAL PLANE

Merloni et al. Falke, Koerding et al.

SUPERLUMINAL MOTIONS IN QSOs & AGN

•OBSERVED IN > 30 QSOs & AGN

•IN RADIO & OPTICAL WAVES

• PROPER MOTION SEEN IN YEARS

•Vapp UP TO 30c in blazars

•One sided because of Doppler boosting

•WHAT IS THE NATURE ?

“PLASMONS” OR SHOCKS ?