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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 - PowerPoint PPT Presentation
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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)
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