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 RemillardKavli Institute for Astrophysics and Space ResearchMassachusetts Institute of Technology

http://xte.mit.edu/~rr/XIVschool_III.2.ppt

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

Hard State of Black Hole Binaries

Hard State: disk fraction fdisk < 20%; power-law photon index, 1.4 < < 2.1;power (0.1-10 Hz) rms > 0.10

steady jet

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)

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)

Hard State Correlates with Radio Emission

Corbel et al. 2000

why a Jet?(Fender 2006)

• flat radio index(like AGN)

• polarized

• jet images in Cyg X-1 (weak constraint) and inGRS 1915+105 (highly collimated to AU scales;

Dhawan et al. 2000)

Radio Flux vs. X-ray Flux (Hard State to Quiescence)

Gallo, Fender, & Pooley 2003; elevated to “Fundamental Plane of Black HoleActivity” (with AGN and mass corrections; Merloni, Heinz, & DiMatteo 2005)

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)

Modeling the Hard State

Key Questions:• relativistic jet?Need better measurements of collimation, energy, and outflow speed in hard state.

• alternative techniques to measure RinProbe 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

Temporal Signature of the Hard State

GX339-4: average PDS across SPL:hard transition

Broad feature near 1 Hz: signature of a steady jet

Relativistic Impulsive Jets from BHBs

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

Radio Interferometry: GRS1915+105

“Unified Model for Jets in Black Hole Binaries”

Fender, Belloni, & Gallo 2004

Hard Color

X-rayintensity

Remillard 2005

States of Black Hole Binaries

steep power law state:

photon index > 2.4 ;

rms < 0.15 ;

disk frac. fdisk < 80% + QPOs or fdisk< 50% + no QPOs

Energy spectra Power 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

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)

Steep Power Law StateHeritage:

• “Very High State” (only 2 sources: Miyamoto et al. 1991; 1993)

• Gamma Bright State (Grove et al. 1998)

blackbody energetics

SPL

|

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

Comparing SPL vs. Thermal States

High Frequency QPOs (40-450 Hz)

HFQPO stability

Variable peaks constant to few % outliers shift to 15%

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

Preferred HFQPO Frequencies

GR Coordinate Frequencies

r, = f ( Mx, a*, r) (r in units of GMx/c2)

= c3/GMx [ 2 r 3/2 (1+ a* r -3/2) ]-1

r = || (1 - 6r -1 + 8a* r -3/2 - 3a*2 r -2)1/2

= || (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

HFQPOs and General Relativity

HFQPO frequency () and GR dynamical frequencies:

• Easy to measurefew percentimmune to (d, Av , i ))

• Long reach: X-rays penetrate ISM better than optical

Page & Thorne 1974Merloni et al. 1999

Greene et al. 2001Strohmayer 2001Remillard et al. 2002Shafee et al. 2006

High Frequency QPOs

source HFQPO (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-------

High Frequency QPOs

source HFQPO (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

HFQPO Frequencies vs. BH Mass

GROJ1655, XTEJ1550,

and GRS1915+105

qpo at 2o: o = 931 Hz / Mx

Same QPO mechanism and similar value of a*

Compare subclasses

while model efforts continue

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, }

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)

HFQPO Conclusions

HFQPOs are a compelling theme for GR-study of BHBs QPO ~ dynamical frequencies of disk for R < 10 Rg Stable (1st order) for each BH, despite large changes in Lx 3:2 ratio for HFQPO pairs in 4 BHBs common mechanism? Roughly ~ 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

Black Hole States: Statistics

XTE J1550-564 GRO J1655-40 XTE J1118+480

Steep Power Law 26 15 0Thermal 147 47 0Low/hard 22 2 10

Intermediate 57 2 0

Timescales (days) for state (all BH Binaries)

duration transitionsSteep Power Law 1-10 <1Thermal 3-200 1-10Low/hard 3-200 1-5

Intermediate 3-30 1-3

BH States: Overview

GRO J1655-40

1996-97 outburst

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

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)

Steep Power Law

Intermediate O

BH States: Overview

GX339-4

Mx = 5 – 15 Mo

Frequent outbursts: 1970 - 2005+ extended, faint, hard states

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

BH States: Overview

H1743-322

Mx unknown (ISM dust)

HEAO-1 outburst: 1977RXTE: 2003; minor outburst 2005

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

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.

Appendix 1: Low Frequency QPOs (0.05-30 Hz)

XTE J1550-5641998 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)

Appendix 1: Low Frequency QPOs : Subtypes

Type: A B CPhase Lag: soft hard near zero (Hz): ~8 ~6 0.1 – 15a (rms %) few few 5 – 20 Q : 2 – 3 ~10 ~10State: SPL SPL Hard/Int.

HFQPO coupling yes, 3o yes, 2o no HFQPOs

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

XTEJ1550-564

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)

Appendix 1: QPO Frequency vs. Disk Flux

? different types of magnetized disk ?

Appendix 2: HFQPO Overview: GRO J1655-40 (1996)

67 observations10 HFQPO detections

X-ray states:

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

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

HFQPO Overview: GRO J1655-40 (2005)

450 observations6 HFQPO detections

X-ray states:

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

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

HFQPO Overview: XTE J1550-564 (1998)

202 observations 16 HFQPO detections

X-ray states:

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

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

HFQPO Overview: XTE J1550-564 (2000)

63 observations6 HFQPO detections

X-ray states:

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

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

HFQPO Overview: XTE J1859+226 (1999)

130 observations5 HFQPO detections

X-ray states:

Thermal x

Hard (jet)

Steep Power Law

Intermediate O

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