1. Service d’Astrophysique, CEA/Saclay (France)
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)

2. PLAN Introduction to microquasars The X-ray binary systems
Different binary systems
Variability: light curves, changes in states
The different types of jets
Compacts jets
Isolated and superluminal ejections
Large scale jets: interaction with the surrounding medium
ex: SS433/W50 and XTE J
Comparison to extragalactic jets
Microblazars: candidates
Microquasars: sources of TeV Neutrinos ?
Conclusion

3. I. Introduction to Microquasars

4. QUASARS  MICROQUASARS
Quasar 3C 223
Microquasar 1E
VLA at 1477MHz ~ 20 cm
radio (VLA) observations at 6 cm
Mirabel et al. 1992

5. MICROQUASARS : ARTIST’S VIEW

6. MICROQUASAR / QUASAR / GRB ANALOGY

7. EMISSIONS FROM A MICROQUASAR
Compacts jets
Radio  IR
 X?
(synchrotron)
Donor star
IR  UV
(thermal)
Disc
+ corona ?
X  IR
therm + non therm
Wind
Visible  radio
(free-free) M •
Large scale ejection
Radio & X
Interaction with environment
Dust ?
IR  mm
(thermal)

8. II. The X-ray binary systems

9. DIFFERENT BINARY SYSTEMS
type of the donor star  type of accretion (wind or Roche lobe overflow)
very different scales:
J.A. Orosz
Every X-ray binary is a possible microquasar!

10. VARIABILITY Variations = changes in the state of the source
GX339-4 lightcurve
Variations = changes in the state of the source
lightcurves:
GX / GRS
 Variations on very different time scales !
 “easy” observations for human time scale
1996
2003
GRS
X (2-10 keV)
Radio (2,25 GHz)
Rau et al (2003)

11. VARIABILITY : state changes
“Classically” : soft X-rays  disc (thermal), hard X-rays  corona (IC of therm. phot.)
Some state changes  transient ejections, ex: off  high/soft
Radio & X-ray spectrum
Accretion disc
Radio jet •
compact jets
radio – hard X-ray correlation
 states // radio quiet / loud AGNs?
Fender (2001)

12. accretion / ejection coupling
Mirabel et al (1998)
Marscher et al (2002)
cycles of 30 minutes in GRS :
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 !

13. III. The different types of jets

14. COMPACTS JETS
Observations : image in radio (difficult: mas. !) or spectrum: radio flat (easier)
Dhawan et al. (2000)
Fuchs et al. (2003)
flat spectrum
GRS
GRS
flat or inverted spectrum model:
conical jet  cut  1/Rmin
shock accelerated e-
optically thick synchrotron emission from radio  IR
optically thin synchrotron in X-rays ?
Falcke et al. (2002)

15. SUPERLUMINAL EJECTIONS
 same Lorentz factor as in Quasars :  ~ 5-10
VLBI at 22 GHz ~ 1.3 cm
VLA at 3.5 cm
~ arcsec. scale
~ milliarcsec. scale
Mirabel & Rodriguez (1994)
Move on the sky plane ~103 times faster
Jets are two-sided (allow to solve equations  max. distance)

16. 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 1E
GRS
VLA
at 6 cm

17. JETS AT LARGE SCALES ex: SS 433 / W50
Vermeulen et al. (1993)
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 !

18. W50 relativistic ejections at arcsec.-scale
associated to thermal X-ray emission
(Migliari et al. 2002)
the radio nebula W50 : SN remnant
elongated shape (2°x1°~120pc x 60pc)
due to jets ?
Large scale X-ray jets but no motion observed
East part: non-thermal X-ray emission maybe due to jet / ISM interaction
W50
Radio + X-ray
2° ~120 pc
SS 433
W50 : > 104 years
PJ ~ 1039 erg/s
Ec ~ 1051 erg
Dubner et al. (1998)

19. LARGE SCALE JETS ex: XTE J1550-564
20 Sept. 1998: strong and brief X-ray flare
Mbh= /- 1.0 M ; d ~ 5 kpc (Orosz et al. 2002)
RXTE/ASM lightcurve ( )
2 –10 keV
VLBI
20 Sept. 1998
one day X-ray flare
Hannikainen et al (2001)
Superluminal relativistic ejection (Hannikainen et al. 2001)

20. XTE J1550-564 : LARGE SCALE X-RAY JETS !
Chandra images keV
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 ?
23 arcsec 

21. 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 ?

22. Comparison with extragalactic jets
Microquasars :  ~ 1.04 – 30 LJ ~ 1038 – 1040 erg.s Ld ~ 1036 – 1039 erg.s-1
Quasars :  ~ 2.5 – LJ ~ 1043 – 1048 erg.s Ld ~ 1042 – 1047 erg.s-1
3C273: quasar (z=0.158)
Pictor A: radio galaxy FR II
radio
Optical (HST)
X-ray
Chandra image + radio (20 cm) contours
Wilson et al. (2001)
XTE J
Marshall et al. (2001)
SS433/W50

23. Spectrum of a Quasar thermal (disk) inverse Compton (jet)
Jets are the only truly broad-band sources in the universe (radio-TeV)!
thermal (disk)
inverse Compton (jet)
Synchrotron (jet)
Lichti et al. (1994)

24. Spectrum of a Microquasar
If jet emission extends up to the visible band, the jet has > 10% of the total power
thermal (disc)
Synchrotron (jet) ?
MeV emission due to Synch. Self-Compton from the compact jet ?
GeV ? (GLAST)
shocks with the ISM TeV ?
Synchrotron (jet)
Markoff et al. (2001)
If jet emission dominates the X-ray band, the jet has > 90% of the total power

25. MICROBLAZARS Microblazars = sources with viewing angle < 10°:
- time scales lowered by 22
- flux density increased by 83
 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)

26. IV. Microquasars: sources of TeV Neutrinos ?

27. Radio Cores: particle accelerators and high energy laboratories
Blazars emit:
511 keV annihilation line
Gamma-rays
TeV emission
TeV neutrinos
 microblazars ?

28. 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 TeV neutrino emission
 Should precede the radio flares associated with major ejection events
 Detection of neutrinos = diagnostic of hadronic jets _

29. Neutrino flux predictions for Microquasars
see Distefano et al., ApJ, 2002
Predicted number of muon events in a km2 detector (for E > 1 TeV):
background
 employing jet parameters
inferred from radio observations
of various ejection event
! Large uncertainties !
! Jet power overestimated by
a factor of ~
 detection
+ microblazars: should emit
neutrinos with larger flux
 a way of identification

30. CONCLUSIONS PROSPECTS Astrophysics Particle Physics
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