ARTIST VIEW OF BLACK HOLES

by

Jean-Pierre Luminet

ACCRETION/JET CONNECTION IN MICROQUASARS:AS IN AGN THE JETS COME IN DIFFERENT TYPES

1) DOUBLE-SIDED RADIO SOURCE WITH STATIONARY LOBES

ASSOCIATED TO PERSISTENT X-RAY SOURCES

2) DOUBLE OR SINGLE SIDED MOVING JETS THAT APPEAR AT

TRANSITIONS FROM LOW-HARD TO HIGH-SOFT X-RAY STATES.

FORMATION OF TERMINAL LOBES AT RADIO & X-RAYS.

3) TRANSIENT “BABY-JETS” DURING FAST TRANSITIONS FROM

LOW-HARD TO HIGH SOFT STATES. FLUENCE-T CONNECTION ?

4) COMPACT STEADY JETS DURING LONG LOW-HARD STATES

SEEN IN ALL STEADILY ACCRETING BHs: Cyg X-1… Sgr A*

IN QSOs ASSOCIATED TO SPECIFIC X-RAY STATES

X/GAMMA-RAY SPECTRA OF BLACK HOLE BINARIESX/GAMMA-RAY SPECTRA OF BLACK HOLE BINARIES GRO (Grove et al 98)

DIFFERENT FROM SPECTRA OF NEUTRON STAR X-RAY BINARIES

Grebenev et al. 93

Low/Hard and High/Soft states in Black HolesLow/Hard and High/Soft states in Black Holes

Accretion disk structure and spectrum described by Shakura & Sunyaev 73

Compact jet Corbel et al. 2001

The Power-Evolution of Black Hole XRBs

Accretion DiskRadio & X-ray Spectrum Radio JetM

Fender (2001)Fender (2001)

SunyaevSunyaev

SunyaevSunyaev

SunyaevSunyaev

Falcke et al. & Fender et al. 2002

X-RAY STATES AND JETS

•MAJOR EJECTIONS TAKE PLACE DURING X-RAY TRANSITION FROM LOW-HARD TO HIGH-SOFT STATE (Mirabel et al. 1994, 1998; Fender et al. 2002).

Microquasar GRS 1915+105

VLBA ALLOWS ASTROMETRY AND PROPER MOTIONS WITH SUB-MAS PRECISION !

(Pooley with Ryle)

RXTE 100

AU

Dhawan, Mirabel, Rodriguez, 2000

MICROQUASARS AS PROBES OF BLACK HOLE FORMATION

HOW ARE STELLAR-MASS BLACK HOLES FORMED ?

IS IT BY PROMPT COLLAPSE OR DELAYED/FAILED COLLAPSE ?

ARE BLACK HOLES BORN WITH NATAL KICKS AS NEUTRON STARS ?

IS THIS A FUNCTION OF THE PROGENITOR AND BLACK HOLE MASS ?

ANSWERS ARE IMPORTANT TO: 1) CONSTRAIN THE PHYSICAL MODELS,

2) FOR ASTRONOMY PROJECTS THAT USE GRB’s FOR COSMOLOGY.

IS THE FORMATION OF BH’s ALWAYS ASSOCIATED TO SN AND GRB’s ?

THE BIRTH PLACE AND MECHANISM OF FORMATION CAN BE

INFERRED FROM THE KINEMATICS. BUT IT IS NOT POSSIBLE

TO KNOW THE SPACE VELOCITY OF SOLITARY BLACK HOLES.

MULTIWAVELENGTH TOOLS TO TRACK THE PATH OF MICROQUASARS

1) RADIAL VELOCITY OF THE CENTRE OF MASS

FROM SPECTROSCOPY OF THE DONOR STAR

2) PROPER MOTION FROM ASTROMETRY OF

COMPACT JETS (VLBI) OR DONOR STAR (OPTICAL)

THE GALACTOCENTRIC ORBIT CAN THEN BE

COMPUTED USING A GALACTIC MASS MODEL

3) DISTANCE BY CLASSIC METHODS IN ASTRONOMY

BLACK HOLE IN THE HALO Mirabel , Dhawan , Rodrigues, Mignani, Guglielmetti (Nature, September 13, 2001)

XTE J1118+480: MBH=7 M @ l=158o b=+62o; D=1.9 kpc

Vpec=150 km/sec

Proper Motions:

Radio with VLBA

Optical on 43 years POSS

DRIFTING AT A VELOCITY OF 150 km/sec

Animacion

POPULAR VIEW

OF BLACK HOLES

AS

“CANNIBAL STARS”

Irapuan

THE PATH OF SCORPIUS X-1

A GALACTIC BULGE X-RAY BINARY WITH A “CHAOTIC” ORBIT

THE RUNAWAY BLACK HOLE GRO J1655-40 (Mirabel, Rodrigues, et al. 2002)

DISTANCE = 1-3 Kpc

RUNAWAY VELOCITY:

116 +/- 12 km/sec

LINEAR MOMENTUM =

550 +/- 100 MSUN km/s

as neutron stars

BH FORMED IN A SN

Consistent with

(Israelian et al. Nature 2001)

PROPER MOTION WITH HST

THE BIRTH SITES OF HMXBs LSI +61 303 Cygnus X-1

Rodrigues & Mirabel 2003

THE AGES, RUNAWAY VELOCITIES, PROGENITOR MASS LIMITS ETC…

CAN BE CONSTRAINED

RESULTSIn proceedings of 4th Microquasar workshop

•ON 7 INDIVIDUAL SOURCES. THE RUNAWAY KINETIC ENERGY OF

X-RAY BINARIES IS < 1% OF THE KINETIC ENERGY OF SUPERNOVAE.

ALTHOUGH THE SAMPLE IS STILL NOT STATISTICALLY SIGNIFICANT

TO DRAW MUCH GENERAL CONCLUSIONS.

•IN THE FUTURE IT WILL BE POSSIBLE TO CONSTRAIN WITH MORE

PRECISION WHICH BLACK HOLES ARE FORMED IN THE EXPLOSION

OF MASSIVE STARS AND WHICH ARE FORMED BY IMPLOSION,

AS A FUNCTION OF THE PROGENITOR AND BLACK HOLE MASSES.

•CAVEAT: SELECTION EFFECT IN THE SAMPLE BECAUSE THE MOST

ENERGETIC NATAL EXPLOSIONS MAY UNBOUND THE BINARIES,

AND THEREFORE NOT ABLE TO SEE THOSE HIGH SPEED REMNANTS.