1. XIV Advanced School on Astrophysics Topic III: Observations of the Accretion Disks of Black Holes and Neutron Stars III.2 X-ray States of Black Hole Binaries (II)
Ron Remillard
Kavli Institute for Astrophysics and Space Research
Massachusetts Institute of Technology Ok

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 fraction fdisk < 20%;
power-law photon index, 1.4 < G < 2.1;
power ( 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 ~ Rg
lower radiative efficiency
(energy advected into BH)
electrons radiate synchrotron and inverse Compton
predicts convection and outflow
XTE J (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 GRS (Belloni et al. 1997)
…. and in optical continuum cutoff of quiescent state of A
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 (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)
XTEJ 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 spectrum broad 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: GRS
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 GRS

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

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 spectra Power density spectra
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 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 [ 2p r 3/2 (1+ a* r -3/2) ]-1
nr = |nf| (1 - 6r a* r -3/2 - 3a*2 r -2)1/2
nq = |nf| (1 - 4a* r -3/2 + 3a*2 r -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 ; n immune 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 J , 276
GRS , 67, 113, 168
XTE J
4U broad features (Klein-Wolt et al. 2003)
XTE J
H , 242

22. High Frequency QPOs 4 HFQPO pairs with frequencies in 3:2 ratio
source HFQPO n (Hz)
GRO J , 450
XTE J , 276
GRS , 67, 113, 168
XTE J 4U
XTE J
H , 241
4 HFQPO pairs with frequencies in 3:2 ratio

23. HFQPO Frequencies vs. BH Mass
GROJ1655, XTEJ1550,
and GRS
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 ; 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 J GRO J XTE J
Steep Power Law
Thermal
Low/hard
Intermediate
Timescales (days) for state (all BH Binaries)
duration transitions
Steep Power Law <1
Thermal
Low/hard
Intermediate

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

28. + 3 faint hard-state outbursts 2001, 2002, 2003
BH States: Overview
XTEJ
Mx = 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. + extended, faint, hard states
BH States: Overview
GX339-4
Mx = 5 – 15 Mo
Frequent outbursts:
+ extended, faint, hard states
Thermal x
Hard (jet) g
Steep Power Law D
Intermediate O

30. BH States: Overview H1743-322 Mx unknown (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 J
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
XTEJ
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): ~ ~ – 15
a (rms %) few few – 20
Q : – ~ ~10
State: SPL SPL Hard/Int.
HFQPO coupling yes, 3no yes, 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)