Ron Remillard Kavli Institute for Astrophysics and Space Research

1. XIV Advanced School on AstrophysicsTopic III: Observations of the Accretion Disks of Black Holes and Neutron StarsIII.2 X-ray States of Black Hole Binaries (II) Ron Remillard Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology http://xte.mit.edu/~rr/XIVschool_III.2.ppt

2. III.2 X-ray States of Black Hole Binaries (II) • Hard State (and Quiescence) • Hard State Definition • Advection and Jet Models for the Hard State • Impulsive Jets at State Transitions • Alternative Views of Black Hole X-ray States • Steep Power Law State • Summary of Properties • Concepts to Explain the Steep Power Law Spectrum • Quasi-Periodic Oscillations (QPOs) • Overviews of Black Hole States • Statistics of State Occupation and Parameter Distributions • Overviews Diagrams for States and High-Frequency QPOs

3. Hard State of Black Hole Binaries Hard State: disk fractionfdisk < 20%; power-law photon index, 1.4 < G < 2.1; power (0.1-10 Hz) rms > 0.10 steady jet  

4. Modeling the Hard State • ADAF model: • (Advection-Dominated Accretion Flow) • (Narayan lecture today!) • transition: Keplerian to quasi-radial inflow at ~100-500 Rg • lower radiative efficiency • (energy advected into BH) • electrons radiate synchrotron and inverse Compton • predicts convection and outflow XTE J1118+480 (low NH)….truncated, cool disk (McClintock et al. 2001)

5. Modeling the Hard State • ADAF model: • Other evidence of truncated disks: • Apparent cool, large, disks in hard states of other sources (e.g. cygx1) • …. in some instability cycles of GRS1915+105 (Belloni et al. 1997) • …. and in optical continuum cutoff of quiescent state of A0620-00 • Controversy: Real or appearances?? • Profile of broad Fe line (Miller et al. 2004)  “only appearances” • (in limited observations)

6. Hard State Correlates with Radio Emission • why a Jet? • (Fender 2006) • flat radio index • (like AGN) • polarized • jet images in Cyg X-1 (weak constraint) and in • GRS 1915+105 (highly collimated to AU scales;Dhawan et al. 2000) Corbel et al. 2000

7. Radio Flux vs. X-ray Flux (Hard State to Quiescence) Gallo, Fender, & Pooley 2003; elevated to “Fundamental Plane of Black Hole Activity” (with AGN and mass corrections; Merloni, Heinz, & DiMatteo 2005)

8. Modeling the Hard State • Jet-based models • Synchrotron • (Markoff et al. 2001) • Synchrotron/Compton • (Markoff, Nowak, & Wilms 2005) • Kalemci et al. 2005 • ADAF/JET Hybrid • (Yuan, Cui, & Narayan 2005) XTEJ1118+480 synchrotron model (Markoff et al. 2001) Compton model (Frontera et al. 2001)

9. Modeling the Hard State • Key Questions: • relativistic jet? • Need better measurements of collimation, energy, and outflow speed in hard state. • alternative techniques to measure Rin • Probe inner disk radius (e.g., Fe line, power continuum, e.g. Uttley et al. 2008) • explain power density spectrumbroad power peak near 1 Hz in hard state

10. Temporal Signature of the Hard State GX339-4: average PDS across SPL:hard transition Broad feature near 1 Hz: signature of a steady jet

11. Relativistic Impulsive Jets from BHBs Radio Interferometry: GRS1915+105 • Impulsive Jets • Ejecta v/c > 0.9 for several sources; jet content unknown • Seem to occur at state transitions • Correlated to giant X-ray flares (hours) near start of outbursts • X-ray jet seen year later at ISM contact, for 2 sources • Smaller impulsive jets seen with correlated X-ray flares during instability cycles in GRS1915+105

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

13. States of Black Hole Binaries steep power law state: photon index G > 2.4 ; rms < 0.15 ;disk frac. fdisk < 80% + QPOs or fdisk< 50% + no QPOs Energy spectraPower density spectra 1 10 100 .01 .1 1 10 100 Energy (keV) Frequency (Hz) Neutron stars(atoll type) have soft (thermal) and hard states, but they never show SPL-dominated spectra

14. States of Black Hole Binaries • Origin of steep power law? • Radiation mechanism? : inverse Compton (widely assumed) • Energy source?: disk • Source of e- acceleration?: (rough concepts) • Plunging region (R < RISCO) (e.g., Titarchuk & Shrader 2002) • Effects of a fully magnetized disk (e.g., Tagger & Pellat 1999) • Mechanism for QPOs?: • “centrifugal barrier oscillations” (Chakrabarti et al. 2000) • magnetic spiral waves (Rodriguez et al. 2002)

15. Steep Power Law State • Heritage: • “Very High State” (only 2 sources: Miyamoto et al. 1991; 1993) • Gamma Bright State (Grove et al. 1998) blackbody energetics SPL |

16. Comparing SPL vs. Thermal States • Why do we need 2 soft states for BH systems? Accretion disk theory (thermal state) does not naturally provide: • Coronae of 30 keV to 1 MeV • Means to convert up to 90% of the energy into this corona • Frequent and variable QPOs at 0.1-30 Hz • Conclusions: • Do not combine thermal and SPL  “soft” • 3 X-ray States  3 Accretion Systems

17. High Frequency QPOs (40-450 Hz)

18. Preferred HFQPO Frequencies HFQPO stability Variable n ? peaks constant to few % outliers shift to 15% n correlation 3:2 ratio X-ray state Steep Power Law Luminosity span factors ~ 3-6 ------ Miller at al. 2001 Remillard et al. 2002; 2006 Homan et al. 2005; 2006

19. GR Coordinate Frequencies nr, q, f = f ( Mx, a*, r) (r in units of GMx/c2) nf = c3/GMx [ 2pr3/2 (1+ a*r-3/2) ]-1 nr = |nf| (1 - 6r-1 + 8a*r-3/2 - 3a*2r-2)1/2 nq = |nf| (1 - 4a*r-3/2 + 3a*2r-2)1/2 see Merloni et al. 1999 Investigated for neutron star QPOs by Stella et al. 1999

20. HFQPOs and General Relativity HFQPO frequency (n) and GR dynamical frequencies: Page & Thorne 1974 Merloni et al. 1999 Greene et al. 2001 Strohmayer 2001 Remillard et al. 2002 Shafee et al. 2006 • Easy to measure (sn / n ~ few percent ; nimmune to (d, Av , i )) • Long reach: X-rays penetrate ISM better than optical

21. 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 -------

22. 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

23. 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

24. 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)…. Disputed? • Torus Models (Rezzolla et al. 2003; Blaes, Arras, & Fragile 2006) • AEI + Rossby vortex (Tagger & Varniere 2006)

25. HFQPO Conclusions • HFQPOs are a compelling theme for GR-study of BHBs • QPO n ~ dynamical frequencies of disk for R < 10 Rg • Stable n (1st order) for each BH, despite large changes in Lx • 3:2 ratio for HFQPO pairs in 4 BHBs common mechanism? • Roughly n ~ 1/M for 3 cases with measured pairs plus BH mass • Primary HFQPO Spectral Properties are unexplained • tied to steep power law, when detected • No detections in BHB thermal state • 3rd harmonic is shifted to higher energy and lower Lx • HFQPOs are subtle (rms 0.5 to 6%); need a new mission with effective area >> RXTE

26. 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

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

28. 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

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 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

31. References Most references are in the reviews: McClintock & Remillard 2006, “Compact Stellar X-ray Sources”, eds. Lewin & van der Klis, Ch. 4, also astroph/ Remillard & McClictock 2006, ARAA, 44, 49 Additional References: Blaes, Arras, & Fragile 2006, MNRAS, 369, 1235 Kalemci et al. 2005, ApJ, 622, 508 Markoff, Nowak, & Wilms 2006, ApJ, 635, 1203 Merloni, Heinz, and DiMatteo, ApSpSci, 300, 45 Tagger & Varniere 2006, ApJ, 652, 1457 Uttley et al. 2008, COSPAR paper, in preparation.

32. Appendix 1: 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)

33. Appendix 1: 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

34. Appendix 1: 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)

35. Appendix 1: QPO Frequency vs. Disk Flux ? different types of magnetized disk ?

36. Appendix 2: HFQPO Overview: GRO J1655-40 (1996) 67 observations 10 HFQPO detections X-ray states: Thermal x Hard (jet)g Steep Power Law D Intermediate O

37. PDS by State/Group: GRO J1655-40 (1996)

38. HFQPO Overview: GRO J1655-40 (2005) 450 observations 6 HFQPO detections X-ray states: Thermal x Hard (jet)g Steep Power Law D Intermediate O

39. PDS by State/Group: GRO J1655-40 (2005)

40. HFQPO Overview: XTE J1550-564 (1998) 202 observations 16 HFQPO detections X-ray states: Thermal x Hard (jet)g Steep Power Law D Intermediate O

41. PDS by State/Group: XTE J1550-564 (1998)

42. HFQPO Overview: XTE J1550-564 (2000) 63 observations 6 HFQPO detections X-ray states: Thermal x Hard (jet)g Steep Power Law D Intermediate O

43. PDS by State/Group: XTE J1550-564 (2000)

44. HFQPO Overview: XTE J1859+226 (1999) 130 observations 5 HFQPO detections X-ray states: Thermal x Hard (jet)g Steep Power Law D Intermediate O

45. PDS by State/Group: XTE J1859+226 (1999)