The X-ray States and High Frequency Oscillations of Black Holes Binaries
37
The X-ray States and High Frequency Oscillations of Black Holes Binaries Ron Remillard, MIT Primary Collaborator, Jeff McClintock CfA
description
The X-ray States and High Frequency Oscillations of Black Holes Binaries. Ron Remillard, MIT Primary Collaborator, Jeff McClintock CfA. Outline. Three States of Active Accretion (10 35 > L x > 10 39 erg/s) Frequent, Rapid Transitions ; Distinct Spectral and Timing Properties - PowerPoint PPT Presentation
Transcript of The X-ray States and High Frequency Oscillations of Black Holes Binaries
The X-ray States and High Frequency Oscillations of Black Holes Binaries
Ron Remillard, MIT
Primary Collaborator, Jeff McClintock CfA
Outline
Three States of Active Accretion (1035 > Lx > 1039 erg/s) Frequent, Rapid Transitions ; Distinct Spectral and Timing Properties Quantitative Definitions ; Select Data to test Physical Models 3-state versus 2-state Prescriptions for States
Study Accretion in Strong Gravity Thermal State: Relativistic Accretion Disk Hard State: Steady Radio Jets ; Broad Fe Line Steep Power Law: Poorly Understood; High-Frequency Oscillations
High-Frequency Quasi-Periodic Oscillations Observational Properties Frequency Link to radii, R < 10 Rg
BH Outbursts & States
Companion star: early K III
Mx = 9.6 + 1.2 M
(Orosz et al. 2002)
XTE J1550-564 discovered, Sep. 6, 1998
BH Outbursts & States
X-ray states:
Thermal xHard (jet)
Steep Power Law Intermediate O
Thermal State
Energy spectra Power density spectra State Definition
disk emits > 75% of energythermal power continuum: rms < 0.06
no QPO with rms > 0.005
accretion disk
weakpower law
weak powercontinuum______| |
Hard State
Energy spectra Power density spectra State Definition
thermal
disk energy fraction < 0.2hard state power law spectrum: < 2.1
power continuum rms > 0.1
Broken power law
1 2
Fe line
|______|
strongpower continuum
Steep Power Law StateEnergy spectra Power density spectra State Definition
power law > 2.4
steep power law disk fraction < 0.8QPO (0.1 – 30 Hz)continuum rms < 0.075
thermal
hard state
Steep power law
disk
Fe
Physical Models for BHB StatesEnergy spectra Power density spectra State Physical Model
steep power law
thermal
hard state
Disk + ??
X-ray States: The Movie
X-ray States: The Movie
States of Black Hole BinariesSources “Agreeable” Problems (high % intermediate)
LMC X-3 LMC X-1 (soft, but high rms, G)XTE J1118+480 4U 1630-47 (50% int.; bad fits)GS 1354-64 V4641 Sgr (embedded; highly var.)4U1543-47 GRS1915+105/steady (high rms, G)XTE J1550-564 Cyg X-1 (very cool disk)XTE J1650-500GRO J1655-40GX339-4H1743-322 (gaps between state parameters [4]SL 1746-331 are more frequently occupied XTE J1748-288 in “problem” sources)XTE J1817-330 XTE J1818-245XTE J1859+226XTE J2012+381
Unified Model for Jets in BH Binaries Remillard 2005
Thermal x Hard (jet)
Steep Power Law Intermediate O
Hard Color
Fender, Belloni, & Gallo 2004
BH States: Overview PlotsGRO J1655-40
1996-97 outburst
Thermal x
Hard (jet)
Steep Power Law
Intermediate O
BH States OverviewH1743-322
Mx unknown (ISM dust)
HEAO-1 outburst: 1977RXTE: 2003; smaller 2005+ 5 faint ones 2006-2009
Thermal x
Hard (jet)
Steep Power Law
Intermediate O
BH States Overview4U1543-47
Mx = 10 + 1.2 Mo
Outbursts 2002
Thermal x
Hard (jet)
Steep Power Law
Intermediate O
BH States OverviewXTE J1859+226
Mx = + 1.2 Mo
Outburst 1999
Thermal x
Hard (jet)
Steep Power Law
Intermediate O
BH States OverviewXTEJ1550-564
Mx = 9.6 + 1.2 Mo
Outburst 1998 ; smaller, 2000; + 3 faint hard-state outbursts
2001, 2002, 2003
Thermal x
Hard (jet)
Steep Power Law
Intermediate O
Short-cut to Sates Classification?
80-90% success in regions of plane:Normalized hard color vs. 1-s flickering
Why is Steep Power Law a Distinct Type of Soft State?
Accretion disk theory (thermal state) does not naturally provide:
‘Corona’ of 10 – 500 keV (perhaps higher) Means to convert up to 90% of the energy into a corona Frequent and variable low-frequency QPOs (0.1-30 Hz) High-frequency QPOs > 100 Hz
The SPL is also different from the Hard State:
SPL is radio-dim or radio-off Power-law photon index ~2.5 (vs. 1.7 for hard state) Power-density spectrum lacks the strong rms of the hard state
3-State Prescription vs. Hard/Soft States
Steep Power Law Mechanisms(Inverse Compton scattering is the expected radiation mechanism,
but “a corona of unspecified origin” is inadequate !)
Bulk Motion Comptonization in Plunging Region (Titarchuk 1997; Montanari et al. 2009 ; Titarchuk & Seifina 2009)
… but how do you get 90% energy in the power law?
Shocks at Transition to Radial Flow (S. Charkrabarti 1990; Kinsuck et al. 2010)
… not confirmed by other groups
Strongly Magnetized Disks (vs. weakly magn. MRI in thermal state)Mag. Spiral Waves (Tagger & Pellat 1998; Tagger & Varniere 2006 Fu & Lai 2009)
… can MHD simulations confirm this concept?
High Frequency QPOs (100-450 Hz)
8 Black Hole Binarieswith transient HFQPOs
4 with two QPOs(seldom at the same time)
4 seen solo
several require multiple observations
to gain a single detection
HFQPO stability
Variable constant to 5% outliers can shift 15%
correlation 3:2 ratio
X-ray state Steep Power Law
Luminosity range factors ~ 3-6
Preferred HFQPO Frequencies
High Frequency QPOs
source Frequency(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
H1743-322 166, 242
Cyg X-1 135
-------
High Frequency QPOs
source Frequency(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
Cyg X-1 135
-------
4 HFQPO pairs with frequencies in 3:2 ratio
HFQPO Frequencies vs. BH Mass
o = 931 Hz / Mx
Same QPO mechanism and similar spin
Compare subclasses
while model efforts continue
HFQPO Frequencies vs. BH Mass
+2 BHBs with single HFQPO
(Q~4; broad energy range;
harmonic 2)
Increase Mass accuracy(McClintock et al. ;
CfA and MIT time at Magellan)
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, }
Kluzniak et all. 2005; Horak & Karas 2006; Stuchlik et al. 2008) Resonance with Global Disk Warp (S. Kato 2004)
Torus Models (Rezzolla et al. 2003; Fragile et al. 2005; Bursa 2007; Horak 2008)
Spiral Waves in a Magnetized Disk (AEI) (Tagger & Varniere 2006) p-modes in Magnetized Disks (Fu & Lai 2009)
MHD Simulations and HFQPOs (Y. Kato 2004… retracted ?)with spin-disk tilt (Fragile & Blaes 2009)
HFQPOs and States: GROJ1655-40 (1996)
300 Hz only ; 7-30 keV
both HFQPOs
450 Hz only ; 15-30 keV
Dynamical Frequencies in General Relativity
“Keplerian” frequency
Dynamical Frequencies in General Relativity
polar anglefrequency
Dynamical Frequencies in General Relativity
r radial frequency
ISCOInnermost Stable Circular Orbit
Disk Radiation in General Relativity
Radius of peak emissivity
Page & Thorne 1974
QPO Frequencies
High-frequency QPOs
QPO Frequencies
\High-frequency QPOs
QPO Frequencies
QPOs:168 113 Hz67
67 Hz Detections in GRS1915+105
28 detections > 4 ; stable to 2 Hz over 12 years
Quantitative Applications for General Relativity
Thermal State Relativistic accretion disk theory MHD simulations: viscosity from magneto-rotational instability
Hard State Models for steady jets from accreting black holes Impulsive, relativistic jets while crossing state boundaries Model Fe line profiles to deduce spin MHD simulations: effects of global B-field
Steep Power Law Stable HFQPOs near dynamical frequencies for disk radii, R < 10 Rg
and 3:2 frequency ratio MHD simulations: what seed conditions strongly magnetized disk?
Steep power law spectrum (and HFQPOs) need your attention !
