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STEADY JETS AND TRANSIENT JETS Characteristics and Relationship

Josep M. Paredes. Radio jets and high energy emission in microquasars. STEADY JETS AND TRANSIENT JETS Characteristics and Relationship Max-Planck-Institut für Radioastronomie, 7 th - 8 th April 2010, Bonn. Microquasars: X-ray binaries with relativistic jets.

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STEADY JETS AND TRANSIENT JETS Characteristics and Relationship

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  1. Josep M. Paredes Radio jets and high energy emission in microquasars STEADY JETS AND TRANSIENT JETS Characteristics and Relationship Max-Planck-Institut für Radioastronomie, 7th - 8th April 2010, Bonn

  2. Microquasars: X-ray binaries with relativistic jets XB: A binary system containing a compact object (NS or a stellar-mass BH) accreting matter from the companion star. 299 XB in the Galaxy (HMXB, Liu et al. 2006, A&A 455,1165 and LMXB 2007, A&A 469, 807). HMXBs: (114) Optical companion with spectral type O or B. Mass transfer via decretion disc (Be stars) or via strong wind or Roche-lobe overflow. LMXBs:(185) Optical companion with spectral type later than B. Mass transfer via Roche-lobe overflow. 9 HMXBs 56 LMXBs 299 XB 65(22%) REXBs Maybe the majority of RXBs are microquasars (Fender 2001) At least 15 microquasars

  3. MICROQUASARS IN OUR GALAXY Name System D Porb Mcomp Activity appθ Jet Size Remarks type (kpc) (d) (M) radio (AU) High Mass X-ray Binaries LSI+61303 B0V+NS? 2.0 26.5  p  0.4  10  700 Precession ? V4641 Sgr B9III+ BH ~10 2.8 9.6 t  9.5 LS 5039 O6.5V+NS? 2.9 4.4 1  3 p 0.15 < 81º 10  1000 Precession? SS 433 evolved A?+BH? 4.8 13.1 11± 5? p 0.26 79º ~104 106Precession,Hadronic, X-ray jet Cygnus X-1 O9.7I+ BH 2.5 5.6 10.1 p  40º ~ 40 Cygnus X-3 WNe+BH? 9 0.2  p 0.69 73º ~ 104Radio outbursts Low Mass X-ray Binaries Circinus X-1 Subgiant+NS ~ 6.5 16.6  t > 15 < 5º >104 XTE J1550-564 G8+BH 5.3 1.5 9.4 t 2 ~ 103 X-ray jet Scorpius X-1 Subgiant+NS 2.8 0.8 1.4 p 0.68 44º ~ 40 GRO J1655-40 F5IV+BH 3.2 2.6 7.02 t 1.1 72º85º 8000 Precession ? GX 339-4?+ BH ~ 4 1.76 5.8 ± 0.5 t  < 4000 1E 1740.7-2942 ?+BH ? 8.5? 12.5?  p   ~ 106 XTE J1748-288 ?+BH ? 8 ? > 4.5? t 1.3 > 104 GRS 1758-258 ?+ BH ? 8.5? 18.5?  p   ~106 GRS 1915+105 K-MIII+BH 12.5 33.5 14 ± 4 t 1.2  1.7 66º70º ~10  104Precession?

  4. MQs as high-energy γ -ray sources Theoretical point of view Leptonic models: SSC Atoyan & Aharonian 1999, MNRAS 302, 253 Latham et al. 2005, AIP CP745, 323 EC Kaufman Bernadó et al. 2002, A&A 385, L10 Georganopoulos et al. 2002, A&A 388, L25 SSC+EC Bosch-Ramon et al. 2004 A&A 417, 1075 Synchrotron jet emission Markoff et al. 2003, A&A 397, 645 Hadronic models: Pion decay Romero et al. 2003, A&A 410, L1 Bosch-Ramon et al. 2005, A&A 432, 609

  5. The VHE gamma-ray Sky Map 38 extragalactic 60 galactic LS I+61 303 Cygnus X-1 LS 5039 PSR B1259-63 At HELSI+61303, LS5039 and Cygnus X-3: Fermi and AGILE (E > 100 MeV) Cygnus X-1: AGILE

  6. Large luminosity and strong stellar wind might be a BH if i<25° (Casares et al. 2005) Radio emitters

  7. Stellar Mass Black Hole Cygnus X-1 5 pc (8’) diameterring-structure of bremsstrahlungemitting ionized gas at theshockbetween (dark) jet and ISM. ● HMXB, O9.71+BH VLA VLBA+VLA WSRT Gallo et al. 2005, Nature 15 mas 30 AU Stirling et al. 2001, MNRAS 327, 1273 Martí et al. 1996, A&A 306, 449

  8. Flaring Activity TeV source: Cygnus X-1 INTEGRAL MAGIC Malzac et al. 2008, A&A 492, 527 Albert et al. 2007, ApJ 665, L51 Hard x-rays==> base of the jet(non-thermal e in the hot comptonising medium, McConnell et al. 2002) g-rays==> further away by interaction with stellar wind (shocks located in the region where the outflow originating close to the BH interacts with the wind of the star, Perucho & Bosch-Ramon 2008, A&A 482, 917) ● Strong evidence (4.1s post trial significance) of intense short-lived flaring episode ● Orbital phase 0.9-1.0, when the black hole is behind the star and photon-photon absorption should be huge: flare in the jet?

  9. AGILE 2-years integrated map AGILE 1-day map October 16, 2009 Black circle: optical position Green contour: AGILE 2sig confidence level Sabatini et al. 2010, ApJ 712, L10

  10. RXTE 2-10 keV Swift 15-50 keV Super-AGILE (gray dots)

  11. Soft state Hard state AGILE 2 sig U.L. above 100 MeV A: 2 weeks B: 4 weeks C: 315 d AGILE data flaring episode

  12. Second AGILE detection of a gamma-ray flare from the Cygnus X-1 region (24-25 March 2010) Bulgarelli et al. 2010, Atel 2512 Fermi Public data. V. Zabalza

  13. Strong radio outbursts Cygnus X-3 ● HMXB, WR+NS? Orbital modulation of X-ray emission lines i>60 NS, i<60 BH Vilhu et al. 2009, A&A 501,679 VLBA VLA, 5 GHz • Exhibits flaring to levels of 20 Jy or more • In 1972 was first “caught” flaring above 20 Jy. These events are amongst the best-known examples of observed expanding synchrotron-emitting sources (21 papers in Nature Phys. Sci. 239, No. 95 (1972)) • Modelling Cyg X-3 radio outbursts: particle injection into twin jets Martí et al. 1992, A&A 258, 309 Miller-Jones et al. 2004, ApJ 600, 368 Martí et al. 2001, A&A 375, 476

  14. RXTE ASM 3–5 keV — BATSE 20–100 keV ┼ GBI 8.3 GHz …. Szostek et al. 2008, MNRAS 388, 1001 Strong radio flares occur only when the source is in the soft state If the non-thermal electrons responsible for either the hard X-ray tails or the radio emission during major flares were accelerated to high enough energies then detectable emission in the γ-ray range, e.g., the GeV or TeV band, would be possible. Given that major radio flares indicates the presence of hard X-ray tails, GeV and TeV emission should be searched for during those radio flares.

  15. AGILE Tavani et al. 2009, Nature 462, 620

  16. Fermi Abdo et al. 2009, Science 326, 1512

  17. Jet IC emission >100 MeV γ-ray modulation in Cyg X-3 Anisotropic IC by jet relat. e− with stellar photons along the orbit produces a modulation in the gamma-ray lightcurve (Khangulyan et al. 2008, MNRAS) Jet launched around a BH - moderate bulk relativistic speed - oriented not too far from the light of sight Dubus et al. 2010, MNRAS • The e− emit synchrotron radio beyond the γ-ray emission zone on much larger scales • A shock occurs in the wind because (Perucho et al. 2010, A&A) • - wind mass-loss rate is very large • - orbit very tight Most μqs jets will interact much further away when their pressure matches that of the ISM. Any HE particles will find a much weaker radiation environment and will be less likely to produce a (modulated) IC γ-ray Anisotropic IC e± pair cascade model. The optical depths for γ-rays created inside the binary system are huge. Escape of γ-rays with energies above a few tens of GeV is not very likely. Bednarek, 2010, MNRAS

  18. LS I +61 303 Historical association with a γ-ray source First high-energy (> 100 MeV) COS-B gamma-ray source: CG/2CG 135+01 Hermsen et al. 1977, Nature 269, 494 The radio emitting X-ray binary LS I+61 303, since its discovery as a variable radio source, has been proposed to be associated with the γ-ray source 2CG 135+01 (= 3EG J0241+6103) (Gregory & Taylor 1978, Nature 272, 704) Periodic emission 26.5 days periodicity Radio (P=26.496 d)Taylor & Gregory 1982, ApJ 255, 210; Gregory 2002, ApJ 575, 427 Optical and IRMendelson & Mazeh 1989, MNRAS 239, 733;Paredes et al. 1994 A&A 288, 519 X-raysParedes et al. 1997 A&A 320, L25 HE gamma-rays Abdo et al. 2009, ApJ 701, L123 VHE gamma-rays Albert et al. 2009, ApJ 693, 303

  19. MAGIC Tavani et al. 1998, ApJ 497, L89 EGRET 3EG J0241+6103 0.8-0.5 0.5-0.8 Albert et al. 2006, Sci 312, 1771 Albert et al. 2009, ApJ 693, 303 Fermi 0.5-0.8 19 Fermi MAGIC blue, 0.5-0.7 VERITAS black, 0.5-0.8 Abdo et al. 2009, ApJ 701, L123

  20. LS I +61 303 Accretion onto a compact object (NS or BH) embedded in mass outflow of the B-star Taylor & Gregory 1982, ApJ 255, 210; Taylor et al. 1992, ApJ 395, 268 Non-accreting young pulsar in orbit around a mass-losing B star Powered by the spindown of a young pulsar (Maraschi & Treves 1981, MNRAS 194,1) Revived after the discovery of PSR B1259-63 (Tavani et al. 1994, ApJ 433, L37) Resolved radio emission pointed towards the microquasar scenario(Massi et al. 2001 A&A 376, 217) EVN at 5 GHz MERLIN at 5 GHz

  21. Jet-like features have been reported several times, but show a puzzling behavior (Massi et al. 2001, 2004). VLBI observations show a rotating jet-like structure(Dhawan et al. 2006, VI Microquasars Workshop, Como, Setember 2006) VLBA G F H E A I D B C J NOT TO SCALE Observer 3.6cm images, ~3d apart, beam 1.5x1.1mas or 3x2.2 AU. Semi-major axis: 0.5 AU

  22. Pulsar scenario: Interaction of the relativistic wind from a young pulsar with the wind from its stellar companion. A comet-shape tail of radio emitting particles is formed rotating with the orbital period. We see this nebula projected (Dubus 2006, A&A 456, 801). UV photons from the companion star suffer IC scattering by the same population of non-thermal particles, leading to emission in the GeV-TeV energy range Zdziarski et al. 2010, MNRAS Not resolved yet the issue of the momentum flux of the pulsar wind being significantly higher than that of the Be wind, which presents a problem for interpretation of the observed radio structures (as pointed out by Romero et al. 2007).

  23. Romero, Okazaki et al. (A&A 474, 15)apply a “Smoothed Particle Hydrodynamics” (SPH) code in 3D dynamical simulations for both the pulsar-wind interaction and accretion-jet models. Pulsar Be star When orbital effects are included, even the most favourable assumptions toward a large Be/pulsar wind momentum ratio do not produce the simple elongated shape inferred in the VLBI radio image, which was previously cited as strong evidence in favour of a pulsar wind interaction scenario 6.7yr GBI data Periodic outbursts: two consecutive outbursts (opt. thick and opt. thin) Shock-in-jet model: The opt. thin spectrum is due to shocks caused by relativistic plasma (transient jet) traveling through a preexisting much slower steady flow (steady jet) Massi & Kaufman Bernadó 2009, ApJ 702, 1179 Lense-Thirring precession induced by a slowly rotating compact object could be compatible with the daily variations of the ejecta angle observed in LS I +61◦303. Massi & Zimmermann 2010 (arXiv:1003.3693)

  24. LS 5039 HESS 3EG J1824-1514 EGRET VLBA+VLA, 5 GHz Aharonian et al. 2005 , Science 309, 746 Paredes et al. 2000, Science 288, 2340 3.9 day orbital modulation in the TeV g-ray flux ● HMXB, O6.5V+NS? Aharonian et al. 2006, A&A 460, 743 The γ-ray data require a location of the production region at the periphery of the binary system at ~1012 cm (Khangulyan et al. 2008, MNRAS; Bosch-Ramon et al. 2008, A&A)

  25. Fermi and H.E.S.S. Fermi Black points (dotted line): phase-averaged spectrum Red points (dotted line): spectrum (fit) at inferior conjunction (0.45-0.9) Blue data points (dotted line): spectrum (fit) at superior conjunction (<0.45 and >0.9) Abdo et al. 2009, ApJ 706, L56

  26. 0.02 0.14 0.27 0.47 0.53 0.75 0.78 0.04 To observer To observer Phase 0 0.5 1 BR127 (2007) GR021 (2000) BP051 (1999) Preliminary! [Moldón et al., in preparation] The orbital plane has two degrees of freedom: Inclination of the orbit Longitude of the ascending node

  27. A new gamma-ray binary? HESS J0632+057 Hinton et al. 2009, ApJ 690, L101 Acciari (for the VERITAS Col.), arxiv:0905.3139 MWC 148: star XMMU J063259.3+0548: open circle Pos. uncertainty of CoG of HESS J0632+057: square marker with error bar • Binary system? • Coincident with Be star MWC 148 • No companion yet detected; no • information on period • Variable X-ray and radio emission Skilton et al. 2009, MNRAS 399, 317

  28. Summary Periodic Periodic Periodic Periodic Periodic • All of them are HMXBs • All of them are radio emitters • All of them have a bright companion (O or B star)  source of seed photons for the IC emission and target nuclei for hadronic interactions • NS and BH are among these detected XRBs • VLBI monitoring of the jets along the orbit is crucial to understand some of these systems • Multi-wavelength (multi-particle) campaigns are of primary importance • HESS J0632+057: New gamma-ray binary?

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