MICROQUASARS JETS:FROM BINARY SYSTEMS TO THE

INTERSTELLAR MEDIUM

(Multi- observations of MICROQUASARS and high energy neutrinos prospects)

Yaël Fuchs

Service d’Astrophysique, CEA/Saclay (France)

PLAN

I. Introduction to microquasars

II. The X-ray binary systems

1. Different binary systems

2. Variability: light curves, changes in states

III. The different types of jets1. Compacts jets

2. Isolated and superluminal ejections

3. Large scale jets: interaction with the surrounding mediumex: SS433/W50 and XTE J1550-564

4. Comparison to extragalactic jets5. Microblazars: candidates

IV. Microquasars: sources of TeV Neutrinos ?

V. Conclusion

I. Introduction to Microquasars

QUASARS MICROQUASARS

Mirabel et al. 1992

Quasar 3C 223 Microquasar 1E1740.7-2942

radio (VLA) observations at 6 cm

VLA at 1477MHz ~ 20 cm

MICROQUASARS : ARTIST’S VIEW

MICROQUASAR / QUASAR / GRB ANALOGY

EMISSIONS FROM A MICROQUASAR

• Donor star IR UV

(thermal)

• Dust ?IR mm(thermal)

• Large scale ejection

Radio & XInteraction with

environment

• Disc + corona ?

X IRtherm + non

therm

• Compacts jetsRadio IR X?

(synchrotron)

• WindVisible radio

(free-free)

M•

II. The X-ray binary systems

DIFFERENT BINARY SYSTEMS• type of the donor star type of accretion (wind or Roche lobe overflow)

• very different scales:

Every X-ray binary is a

possible microquasar!

J.A. Orosz

VARIABILITY

• Variations = changes in the state of the source

• lightcurves: GX 339-4 / GRS 1915+105

Variations on very different time scales !

“easy” observations for human time scale

X (2-10 keV)

Radio (2,25 GHz)

Rau et al (2003)

GX339-4 lightcurve

1996 2003GRS 1915+105

VARIABILITY : state changes

Fender (2001)Fender (2001)

• Accretion discRadio & X-ray spectrum Radio jet

compact jets

“Classically” : soft X-rays disc (thermal), hard X-rays corona (IC of therm. phot.)

Some state changes transient ejections, ex: off high/soft

states // radio quiet / loud AGNs?

radio – hard X-ray correlation

accretion / ejection coupling

• cycles of 30 minutes in GRS 1915+105 : ejections after an X-ray dip disappearance / refilling of the internal part of the disc ? transient ejections during changes of states

same phenomenum in the quasar 3C 120 ? far slower !

Mirabel et al (1998)

Marscher et al (2002)

III. The different types of jets

COMPACTS JETS

GRS 1915+105

Dhawan et al. (2000) Fuchs et al. (2003)

GRS 1915+105

flat spectrum

optically thick synchrotron emission from radio IR

optically thin synchrotron in X-rays ?

flat or inverted spectrum model:conical jet cut 1/Rmin

shock accelerated e-

Observations : image in radio (difficult: mas. !) or spectrum: radio flat (easier)

Falcke et al. (2002)

SUPERLUMINAL EJECTIONS

• Move on the sky plane ~103 times faster• Jets are two-sided (allow to solve equations max. distance)

same Lorentz factor as in Quasars : ~ 5-10

Mirabel & Rodriguez (1994)

VLA at 3.5 cm

VLBI at 22 GHz ~ 1.3 cm

~ arcsec. scale ~ milliarcsec.

scale

JETS AT LARGE SCALES

• Steady jets in radio at arcminute scale

• Sources found to be nearly always in the low/hard state long-term action of steady jets on the interstellar medium

1E1740.7-2942

GRS 1758-258

VLA at 6 cm

JETS AT LARGE SCALES ex: SS 433 / W50

• SS 433 : variable source in radio & X-rays

• distance ~ 3.5 kpc ?

• “moving” lines : enormous Doppler-shifts and period of ~162 days

relativistic jets (0.26c) with precession movement

the 1st microquasar ! (1979)

acceleration of ions !

Vermeulen et al. (1993)

• relativistic ejections at arcsec.-scaleassociated to thermal X-ray emission (Migliari et al. 2002)

• the radio nebula W50 : SN remnantelongated shape (2°x1°~120pc x 60pc) due to jets ?

• Large scale X-ray jets but no motion observedEast part: non-thermal X-ray emission maybe due to jet / ISM interaction

W50

Dubner et al. (1998)

• W50 : > 104 years PJ ~ 1039 erg/s

Ec ~ 1051 erg

W50Radio + X-ray

2° ~120 pc

SS 433

LARGE SCALE JETS ex: XTE J1550-564

• 20 Sept. 1998: strong and brief X-ray flare

• Mbh= 10.5 +/- 1.0 M ; d ~ 5 kpc (Orosz et al. 2002)

RXTE/ASM lightcurve (1998-99)

20 Sept. 1998 one day X-ray flare

Hannikainen et al (2001)

Superluminal relativistic ejection (Hannikainen et al. 2001)

VLBI2 –10 keV

XTE J1550-564 : LARGE SCALE X-RAY JETS !

Chandra images 0.3 - 8 keV

23 arcsec 

Related to the brief flare of Sept. 1998

Discovery of X-ray sources associated with the radio lobes

• Moving eastern source • Alignment + proper motion

First detection of moving relativistic X-ray jets !

Corbel et al. (2002)

• evidence for gradual deceleration• radio-X-ray spectrum: compatible with synchrotron emission from the same e-

distribution

• external shocks with denser medium? Particle acceleration, to TeV ?

SUMMARY ABOUT MICROQUASAR JETS

• compact jets milli-arcsecond

• isolated ejections caused by state changes in the source

sometimes: superluminal ejections 0.1 to 1 arcsecond

• large scale jets: interaction with the interstellar medium

arcminute

• composition ?e-/e+, p+, ions ?

radio Optical (HST) X-ray

Microquasars : ~ 1.04 – 30 LJ ~ 1038 – 1040 erg.s-1 Ld ~ 1036 – 1039 erg.s-1

Quasars : ~ 2.5 – 30 LJ ~ 1043 – 1048 erg.s-1 Ld ~ 1042 – 1047 erg.s-1

Marshall et al. (2001)

3C273: quasar (z=0.158) Pictor A: radio galaxy FR IIChandra image + radio (20 cm) contours

Wilson et al. (2001)

Comparison with extragalactic jets

XTE J1550-564

SS433/W50

Spectrum of a Quasar

Synchrotron(jet)

Synchrotron(jet)

thermal(disk)

thermal(disk)

inverse Compton(jet)

Lichti et al. (1994)

Jets are the only truly broad-band sources in the universe (radio-TeV)!Jets are the only truly broad-band sources in the universe (radio-TeV)!

Spectrum of a Microquasar

If jet emission extends up to the visible band, the jet has > 10% of the total power

Markoff et al. (2001)

If jet emission dominates the X-ray band, the jet has > 90% of the total power

Synchrotron(jet)

Synchrotron(jet)

Synchrotron(jet)

Synchrotron(jet)

thermal(disc)

thermal(disc)

?

• MeV emission due to Synch. Self-Compton from the compact jet ? GeV ? (GLAST)

• shocks with the ISM TeV ?

MICROBLAZARS

• Microblazars = sources with viewing angle < 10°:

- time scales lowered by 22

- flux density increased by 83

intense et rapid variations

CANDIDATES:

• ULXs ? ex: first radio counterpart of an ULX in the NGC 5408 galaxy

• galactic sources?

Cyg X-1: gamma-ray flares observed in this region in 2002

V4641 Sgr: rapid optical flares

high mass X-ray binaries + jet sources

interaction of jet with UV photon field from the donor star inverse Compton

• EGRET unidentified sources ? (LS 5039)

IV. Microquasars: sources of TeV

Neutrinos ?

Radio Cores: particle accelerators and high energy laboratories

Blazars emit:

• 511 keV annihilation line

• Gamma-rays

• TeV emission

• TeV neutrinos

microblazars ?

Neutrino production mechanism in Microquasars

see Levinson & Waxman, Phys. Rev. Letter, 2001

• Hyp: e- / p+ jet• p+ accelerated in the jet to ~ 1016 eV (max En.)• Interaction with:

– Synchrotron photons emitted by shock-accelerated e- if E(p+) > 1013 eV– External X-ray photons from the accretion disc if E(p+) > 1014 eV

photomeson production

pions with ~20% of E(p+)

charged pions decay: + + + e+ + e + +

neutrinos with ~5% of E(p+)

Expected to lead to several hours outburst of 1-100 TeV neutrino emission

Should precede the radio flares associated with major ejection events

Detection of neutrinos = diagnostic of hadronic jets

_

Neutrino flux predictions for Microquasars

see Distefano et al., ApJ, 2002

• Predicted number of muon events in a km2 detector (for E > 1 TeV):

employing jet parametersinferred from radio observationsof various ejection event! Large uncertainties !! Jet power overestimated by a factor of ~ 10-100

detection

background

+ microblazars: should emitneutrinos with larger flux a way of identification

CONCLUSIONS

Advantages of microquasars inspite of their weakness:

• Scales of length and time are proportional to the mass of the black hole shorter phenomena (accretion / ejection link) thus easy to observe for human time scale

• internal accretion disc emits in the X-rays good propagation in the interstellar medium

• Bipolar jets maximum distance

PROSPECTS

• observation of lines composition of the jets !• observation of microblazars ! • gamma-rays observation: TeV ? jets/ISM interaction?

• TeV neutrino detection

Astrophysics Particle Physics