1 / 30

Yaël Fuchs 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). PLAN. Introduction to microquasars The X-ray binary systems Different binary systems

Download Presentation

Yaël Fuchs Service d’Astrophysique, CEA/Saclay (France)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. 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 J1550-564 • Comparison to extragalactic jets • Microblazars: candidates • Microquasars: sources of TeV Neutrinos ? • Conclusion

  3. I. Introduction to Microquasars

  4. QUASARS  MICROQUASARS Quasar 3C 223 Microquasar 1E1740.7-2942 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. Wind • Visible  radio • (free-free) • M • EMISSIONS FROM A MICROQUASAR • Compacts jets • Radio  IR •  X? • (synchrotron) • Donor star • IR  UV • (thermal) • Disc • + corona ? • X  IR • therm + non therm • Large scaleejection • Radio & X • Interaction with environment • Dust ? • IR  mm • (thermal)

  8. II. The X-raybinary systems

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

  10. VARIABILITY GX339-4 lightcurve • Variations = changes in the stateof the source • lightcurves: • GX 339-4 / GRS 1915+105 •  Variations on very different time scales ! •  “easy” observations for human time scale 1996 2003 GRS 1915+105 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 Fender (2001)  states // radio quiet / loud AGNs?

  12. accretion / ejection coupling Mirabel et al (1998) Marscher et al (2002) • 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 !

  13. III. The different types of jets

  14. COMPACTS JETS Observations : imagein radio (difficult: mas. !) orspectrum: radio flat (easier) Dhawan et al. (2000) Fuchs et al. (2003) flat spectrum GRS 1915+105 GRS 1915+105 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. same Lorentz factor as in Quasars :  ~ 5-10 SUPERLUMINAL EJECTIONS 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 actionof steady jets on the interstellar medium 1E1740.7-2942 GRS 1758-258 VLA at 6 cm

  17. Vermeulen et al. (1993) JETS ATLARGE SCALES ex: SS 433 / W50 • SS 433 :variablesource 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 Radio + X-ray 2° ~120 pc 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 SS 433 • W50 : > 104years • 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= 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)

  20. Discovery of X-ray sources associated with the radio lobes • Moving eastern source • Alignment + proper motion 23 arcsec  Related to the brief flare of Sept. 1998 First detection of moving relativistic X-ray jets ! • 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 ? Corbel et al. (2002) XTE J1550-564 : LARGE SCALE X-RAY JETS! Chandra images 0.3 - 8 keV

  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-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 (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 J1550-564 Marshall et al. (2001) SS433/W50

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

  24. thermal(disc) • MeV emission due to Synch. Self-Compton from the compact jet? • GeV ? (GLAST) • shocks with the ISMTeV ? Synchrotron(jet) Synchrotron(jet) ? 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 emissiondominatesthe 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  highmass 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 andhigh energy laboratories • Blazarsemit: • 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 1-100 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 ~ 10-100  detection + microblazars: should emit neutrinos with larger flux  a way of identification

  30. 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 discemits in the X-rays  good propagation in the interstellar medium • Bipolar jets  maximum distance PROSPECTS • observation of lines  composition of the jets ! • observation ofmicroblazars ! • gamma-rays observation: TeV? jets/ISMinteraction? • TeV neutrino detection • Astrophysics Particle Physics

More Related