MICROQUASARS JETS: FROM BINARY SYSTEMS TO THE INTERSTELLAR MEDIUM Multi observations of MICROQUASARS

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MICROQUASARS JETSFROM BINARY SYSTEMS TO THE
INTERSTELLAR MEDIUM (Multi-? observations of
MICROQUASARS and high energy neutrinos
prospects)
Yaël Fuchs Service dAstrophysique, CEA/Saclay
(France)
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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 J1550-564
• Comparison to extragalactic jets
• Microblazars candidates
• Microquasars sources of TeV Neutrinos ?
• Conclusion

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I. Introduction to Microquasars
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QUASARS ? MICROQUASARS
Quasar 3C 223
Microquasar 1E1740.7-2942
radio (VLA) observations at 6 cm
VLA at 1477MHz 20 cm

Mirabel et al. 1992
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MICROQUASARS ARTISTS VIEW
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MICROQUASAR / QUASAR / GRB ANALOGY
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EMISSIONS FROM A MICROQUASAR

• Compacts jets
• Radio ? IR
• ? X?
• (synchrotron)

• Donor star
• IR ? UV
• (thermal)

• Disc
• corona ?
• X ? IR
• therm non therm

• Large scale ejection
• Radio X
• Interaction with environment

• Dust ?
• IR ? mm
• (thermal)

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II. The X-ray binary systems
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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!
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VARIABILITY
GX339-4 lightcurve

• Variations changes in the state of the source
• lightcurves
• GX 339-4 / GRS 1915105
• ? Variations on very different time scales !
• ? easy observations for human time scale

1996
2003
GRS 1915105
X (2-10 keV)
Radio (2,25 GHz)
Rau et al (2003)
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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
Accretion disc
Radio X-ray spectrum
Radio jet

compact jets
radio hard X-ray correlation
Fender (2001)
? states // radio quiet / loud AGNs?
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accretion / ejection coupling
Mirabel et al (1998)
Marscher et al (2002)

• cycles of 30 minutes in GRS 1915105
• 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 !

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III. The different types of jets
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COMPACTS JETS
Observations image in radio (difficult mas. !)
or spectrum radio flat (easier)
Dhawan et al. (2000)
Fuchs et al. (2003)
flat spectrum
GRS 1915105
GRS 1915105
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)
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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)

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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
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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 !

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W50

• relativistic ejections at arcsec.-scale
• associated to thermal X-ray emission
• (Migliari et al. 2002)
• the radio nebula W50 SN remnant
• elongated shape (2x1120pc x 60pc)
• due to jets ?

SS 433

• W50 gt 104 years
• PJ 1039 erg/s
• Ec 1051 erg

Dubner et al. (1998)
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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)
VLBI
2 10 keV
20 Sept. 1998 one day X-ray flare
Hannikainen et al (2001)
Superluminal relativistic ejection (Hannikainen
et al. 2001)
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XTE J1550-564 LARGE SCALE X-RAY JETS !
Chandra images 0.3 - 8 keV
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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 ?

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Comparison with extragalactic jets
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
3C273 quasar (z0.158)
Pictor A radio galaxy FR II
radio
Optical (HST)
X-ray
Chandra image radio (20 cm) contours
Wilson et al. (2001)
XTE J1550-564
Marshall et al. (2001)
SS433/W50
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Spectrum of a Quasar
Jets are the only truly broad-band sources in the
universe (radio-TeV)!
Lichti et al. (1994)
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Spectrum of a Microquasar
If jet emission extends up to the visible band,
the jet has gt 10 of the total power
Markoff et al. (2001)
If jet emission dominates the X-ray band, the jet
has gt 90 of the total power
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MICROBLAZARS

• Microblazars sources with viewing angle lt 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)

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IV. Microquasars sources of TeV Neutrinos ?
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Radio Cores particle accelerators and high
energy laboratories

• Blazars emit
• 511 keV annihilation line
• Gamma-rays
• TeV emission
• TeV neutrinos
• ? microblazars ?

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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) gt 1013 eV
• External X-ray photons from the accretion disc
  if E(p) gt 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

_
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Neutrino flux predictions for Microquasars

• see Distefano et al., ApJ, 2002
• Predicted number of muon events in a km2 detector
  (for E? gt 1 TeV)

background

• ? employing jet parameters
• inferred from radio observations
• of various ejection event
• ! Large uncertainties !
• ! Jet power overestimated by
• a factor of 10-100
• ? detection

microblazars should emit neutrinos with larger
flux ? a way of identification
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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