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Ron Remillard Kavli Center for Astrophysics and Space Research

INPE Advanced Course on Compact Objects Course IV: Accretion Processes in Neutron Stars & Black Holes. Ron Remillard Kavli Center for Astrophysics and Space Research Massachusetts Institute of Technology http://xte.mit.edu/~rr/inpe_IV.2.ppt. IV.2 X-ray States of Black Hole Binaries.

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Ron Remillard Kavli Center for Astrophysics and Space Research

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  1. INPE Advanced Course on Compact ObjectsCourse IV: Accretion Processes in Neutron Stars & Black Holes Ron Remillard Kavli Center for Astrophysics and Space Research Massachusetts Institute of Technology http://xte.mit.edu/~rr/inpe_IV.2.ppt

  2. IV.2 X-ray States of Black Hole Binaries • Thermal States and Accretion Disk Models • Defining States: Energy and Power Density Spectra • Observational Support for the Multicolor Disk Model • Applying Relativistic Disk Models • Hard State, Jets, and Microquasars • Hard State and a Steady Jet • Advection Models (ADAF and CDAF) • Synchrotron/Compton Models • Steep Power-Law of Black Hole Binaries • Summary of Properties • Link to High-Frequency QPOs • Further Considerations of BH X-ray States • Overview of X-ray State Evolution • Alternative Descriptions of X-ray States • Statistics of State Occupations

  3. X-ray States of BHBs • ThermalState: • inner accretion disk

  4. X-ray States of BHBs • ThermalState: fdisk > 75%; rms < 0.075 ; no QPOs (amax < 0.5%) • inner accretion disk

  5. Thermal State Paradigm Theory: Hot gas in thin disk + viscous dissipation Rel. MHD: Plasma + Magneto-Rotational Instability  Thermal radiation ; weakly magnetized disk modified disk blackbody blackbody energetics GR/Keplerian velocities? GX339-4 Relativistic Fe line e.g. Miller et al. 2004; but see Merloni & Fabian 2003 Kubota & Done 2004; Gierlinski & Done 2004 T(r)ar-p; p ~ 0.7 (Kubota et al 2005) (GR tweak of p=0.75)

  6. GR Applications for Thermal State Emissivity vs. Radius in the Accretion Disk Shakura & Sunyaev 1973; Makishima et al. 1986; Gierlinski et al. 1999; Zimmerman et al. 2005 Page & Thorne 1974; Zhang, Cui, & Chen 1997 Gierlinski et al. 2001; Li et al. 2005

  7. GR Applications for Thermal State Relativistic Accretion Disk: Spectral Models • e.g. kerrbb in xspec • Li et al. 2005; Davis et al. 2005 • Integrate over disk and Bn(T) • Correct for GR effects • (grav-z, Doppler, grav-focusing) • Radiative transfer (i.e. f factor)

  8. Thermal state X-ray spectra BH spin • Shafee et al. 2006; Davis, Done & Blaes 2006; McClintock et al. 2006 • Input Mx, d(kpc), disk inclination (i) • Run model trials for values of: • a (viscosity parameter) • model Comptonization (comptt, power-law, broken pow.) • fit hardening factor (h) vs. use Davis and Blaes model • Derive a* (for various trials) in range of Lx

  9. BH spin McClintock et al. 2006

  10. BH spin theory: disk should thicken near Lx ~ 0.3 LEDD McClintock et al. 2006

  11. Thermal state BH spin • Shafee et al. 2006: a* ~ 0.75 for GROJ1655-40, 4U1543-47 • Davis, Done & Blaes 2006: “moderate spin” (0.1-0.8) for XTEJ1550-564, LMC X-3 • McClintock et al. 2006: a* > 0.98 for GRS1915+105 • ------ • Systematic concerns: • Are a-disk assumptions valid? • Theory of radiative transfer (hardening factor) accurate? • ISCO is smeared by B-coupling? • (Page & Throne 1974; Agol & Krolik 2000)

  12. Hard State of BHBs 2. Hard State fdisk < 20%; G ~ 1.4 - 2.1; rms > 0.10 steady jet  

  13. Hard State of BHBs: Steady Radio Jet  2. Hard State fdisk < 20%; G ~ 1.4 - 2.1; rms > 0.10 radio : X-ray correlations: Corbel et al. 2000; Gallo et al. 2003

  14. Hard State of BHBs: Steady Radio Jet Corbel et al. 2000

  15. Hard State of BHBs: Steady Radio Jet GRS1915+105 Oct. 1 – Nov. 7, 1997 X-ray c/s H-ray HR Radio Flux Radio index 50730 50740 50750 MJD

  16. Modeling the Hard State • ADAF models: • (Advection-Dominated Accretion Flow) • transition: Keplerian to quasi-radial inflow at ~100-500 Rg • energy ‘advected’ into BH • electrons can still radiate some synchrotron and inverse Compton • controversies! Model evolution! • ADAF  CDAF (convective DAF)  more outflow XTEJ1118+480 (low NH)….truncated, cool disk (McClintock et al. 2001)

  17. Modeling the Hard State • Hybrid models: • Synchrotron/Compton • (Markoff, Nowak, & Wilms 2005) • Kalemci et al. 2005 • ADAF-fed Syn./Comp.? • (Yuan, Cui, & Narayan 2005) XTEJ1118+480 synchrotron model (Markoff et al. 2001)

  18. States of Black Hole Binaries • 3. steep power law compact corona ? • G > 2.4; rms < 0.15 ; fdisk < 80% + QPOs (or fdisk< 50%) mechanism? : inverse Compton origin? : magnetized disk ? 1 10 100 .01 .1 1 10 100 Energy (keV) Frequency (Hz) Energy spectraPower density spectra Neutron stars(atoll type) have thermal and hard States, but they never show SPL-dominated spectra

  19. Steep Power Law Gamma Ray Bright State (Grove et al. 1998) blackbody energetics SPL |

  20. Physical Models for BHB States Energy spectraPower density spectra Statephysical picture steep power law Disk + ??  thermal hard state Energy (keV) Frequency (Hz)

  21. Comparing SPL vs. Thermal States • Are they different? • Very different X-ray spectra • Extremely Different Gamma Ray Spectra • QPOs vs. none • Conclusions: • Do not combine thermal and SPL  “soft” • 3 X-ray States  3 Accretion Systems

  22. High Frequency QPOs (40-450 Hz)

  23. High Frequency QPOs source HFQPO n (Hz) GRO J1655-40 300, 450 XTE J1550-564 184, 276 GRS 1915+105 41, 67, 113, 168 XTE J1859+226 190 4U1630-472 184 + broad features (Klein-Wolt et al. 2003) XTE J1650-500 250 H1743-322 166, 242 ------- ISCO for 10 Mo BH: nf = 220 Hz (a* = 0.0)  728 Hz (a* = 0.9) Condensations at preferred radii  QPOs (Schnittman & Bertschinger 2004)

  24. High Frequency QPOs source HFQPO n (Hz) GRO J1655-40 300, 450 XTE J1550-564 184, 276 GRS 1915+105 41, 67, 113, 168 XTE J1859+226 190 4U1630-472 184 XTE J1650-500 250 H1743-322 165, 241 ------- 4 HFQPO pairs with frequencies in 3:2 ratio

  25. HFQPO Frequencies vs. BH Mass GROJ1655, XTEJ1550, and GRS1915+105 nqpo at 2no: no = 931 Hz / Mx • Same QPO mechanism and similar value of a* • Compare subclasses while model efforts continue

  26. HFQPOs Mechanisms • Diskoseismology (Wagoner 1999 ; Kato 2001)  obs. frequencies require nonlinear modes? • Resonance in Inner Disk (Abramowicz & Kluzniak 2001). • Parametric Resonance (coupling in GR frequencies for {r, q}Abramowicz et al. 2004 ; Kluzniak et al. 2004; Lee et al. 2005) • Resonance with Global Disk Warp (S. Kato 2004) • MHD Simulations and HFQPOs (Y. Kato 2005) • Torus Models (Rezzolla et al. 2003; Fragile et al. 2005) • GR ray tracing of accretion torus (Bursa et al.) • AEI + Rossby vortex (Tagger & Varniere 2006)

  27. BH Outbursts & States GRO J1655-40 1996-97 outburst Thermal x Hard (jet)g Steep Power Law D Intermediate O

  28. “Unified Model for Jets in BH Binaries” Fender, Belloni, & Gallo 2004 Remillard 2005 X-ray intensity Hard Color

  29. BH States: Overview GX339-4 Mx = 5 – 15 Mo Frequent outbursts: 1970 - 2005 + extended, faint, hard states Thermal x Hard (jet)g Steep Power Law D Intermediate O

  30. BH States: Overview GRO J1655-40 1996-97 outburst Thermal x Hard (jet)g Steep Power Law D Intermediate O

  31. BH States: Overview H1743-322 Mxunknown (ISM dust) HEAO-1 outburst: 1977 RXTE: 2003; minor outburst 2005 Thermal x Hard (jet)g Steep Power Law D Intermediate O

  32. BH States: Overview XTEJ1550-564 Mx = 9.6 + 1.2 Mo Outbursts: 1998 ; smaller, 2000; + 3 faint hard-state outbursts 2001, 2002, 2003 Thermal x Hard (jet)g Steep Power Law D Intermediate O

  33. Black Hole States: Statistics XTE J1550-564GRO J1655-40XTE J1118+480 Steep Power Law 26 15 0 Thermal 147 47 0 Low/hard 22 2 10 Intermediate 57 2 0 Timescales (days) for state (all BH Binaries) durationtransitions Steep Power Law 1-10 <1 Thermal 3-200 1-10 Low/hard 3-200 1-5 Intermediate 3-30 1-3

  34. Low Frequency QPOs (0.05-30 Hz) XTE J1550-564 1998 Sept. 23 QPO: 4 Hz, 12% rms Q ~ 9 Flux 2 Crab (~0.2 LEdd) fdisk = 0.1 QPO wave tracking  random walk in phase (Morgan et al. 1997)

  35. Low Frequency QPOs : Subtypes XTEJ1550-564 Wijnands et al. 1999 Cui et al. 1999 Remillard et al. 2002 Rodriguez et al. 2004 Casella et al. 2005 QPOs across states Jet  INT  SPL ?? diff. mechanism ?? evolution in magnetic instability Type: A B C Phase Lag: soft hard near zero n0 (Hz): ~8 ~6 0.1 – 15 a (rms %) few few 5 – 20 Q : 2 – 3 ~10 ~10 State: SPL SPL Hard/Int. HFQPO coupling yes, 3noyes, 2no no HFQPOs

  36. LFQPO Mechanisms • Periastron precession of emitting blobs in GR (Stella et al. 1999) • Frame Dragging in GR (Stella & Vietri 1998; Fragile et al. 2001) • Resonance oscillation sidebands (Horak et al. 2004) • p-mode oscillations in a truncated disk (Giannios & Spruit 2004) • Inertial-Acoustic oscillations (Milson & Taam 1997) • Global disk oscillations (Titarchuk & Osherovich 2000) • Alfven waves (C.M. Zhang et al. 2005) • Accretion-Ejection Instability in disk (magnetic spiral waves) (Tagger & Pellat 1999) • Radial oscillations in accretion shocks (Molteni et al. 1996; Chakrabarti & Manickam 2000)

  37. QPO Frequency vs. Disk Flux ? different types of magnetized disk ?

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