Transcript Project Status - MIT X-Ray Timing Explorer Project
MIT Workshop on Magnetized Accretion Disks October 19 & 20, 2006
Supported by:
MIT-France Program CEA Saclay, France MIT Kavli Inst. for Astrophysics & Space Research MIT Dept. EE&CS
RXTE
Project
Workshop Handouts & Logistics
Schedule: (4 sessions)
Name Tag
List of Participants
MIT wireless instructions for visitors Thursday dinner? …stay here after session 2 Legal Seafoods? Cambridge Brewery?
X-ray States of Black Hole Binaries: Observations and Physical Models Ron Remillard MIT Kavli Center for Astrophysics and Space Research
Workshop Motivations
Assess status of BH accretion physics General relativity astrophysics at 10 R g ?
X-ray states versus accretion models critical need for steep power-law / QPO paradigm discussions of magnetism in accretion disks
Communicate: observers ; theorists ; GR/MHD physicists 1.5 years since last UCSB program on BH theory informal format for hard results + views & intuitions motivate future work
Active X-ray States of BH Binaries
Thermal State:
thermal spectrum ;
L
a
T 4
; no QPOs Paradigm: Heat from weakly magnetized accretion disk
Hard State:
flat, cutoff power law ; cool disk ; some QPOs Concept: Compton/synchrotron from steady jet (+ ADAF?) Jets are confined by magnetic fields from the disk?
Steep Power Law:
thermal + SPL + QPOs + HFQPOs ?? Magnetized Accretion Disk ; Accretion Torus ??
Black Hole X-ray Nova
GRO J1655-40
First known outbursts: 1994-95; ( ) 1996-97; 2005 Dynamical black hole binary 6.3 ( + 0.5) M o Relativistic Jets in 1994 ~Radio-quiet, 1996-97, 2005
Black Hole X-ray Nova
GRO J1655-40
Different X-ray States
Observation Reviews & Global Studies
Done & Gierlinski 2003 Fender 2006 Fender & Belloni 2004 Charles & Coe 2006 McClintock & Remillard 2006 Psaltis 2006 Remillard & McClintock 2006 van der Klis 2006 Zdziarski & Gierlinski 2004
MNRAS
, 342, 1041
Compact Stellar X-ray Sources
, Ch. 9
ARAA
, 42, 317
Compact Stellar X-ray Sources
, Ch. 5
Compact Stellar X-ray Sources
, Ch. 4
Compact Stellar X-ray Sources
, Ch. 1
ARAA
, 44, 49
Compact Stellar X-ray Sources
, Ch. 2
PThPS
, 155, 99
X-ray States of BHBs
1.
Thermal State:
f
disk > 75%;
rms
< 0.075 ; no QPOs (
a max
< 0.5%)
inner accretion disk
X-ray States of BHBs
1.
Thermal State:
classical disk model:
T(r) ~ r -3/4
L(r) ~ r -2
Heat from Accretion Disk ?
modified disk blackbody blackbody energetics GR/Keplerian velocities?
GX339-4 Relativistic Fe line
T(r)
a
r -p
;
p
~ 0.7 (Kubota et al 2005) (GR tweak of p=0.75) Kubota & Done 2004; Gierlinski & Done 2004 e.g. Miller et al. 2004; but see Merloni & Fabian 2003
Thermal State Paradigm ?
Spectral shape and luminosity evolution consistent with thermal-disk model: Hot gas in Keplerian orbits + efficient dissipation GR/MHD Simulations: Plasma + Magneto-Rotational Instability (MRI): ~Keplerian orbits ; high b =
P
gas / (
B
2 /8 p )
Thermal Radiation from a Weakly Magnetized Disk Alternatives:
low b inner disk (external seed
B
) ?
Plasma Rings (Coppi & Rousseau 2006 ) ?
GR MHD: Stronger jets with higher spin ?
Other X-ray states?
Hard State of BHBs
2. Hard State
f
disk < 20%; G ~ 1.4 - 2.1;
rms
> 0.10
steady jet
(radio emission: collimated, polarized, flat spectrum)
Hard State of BHBs: Steady Radio Jet
2. Hard State
f
disk < 20%; G ~ 1.4 - 2.1;
rms
> 0.10
steady jet
(radio : X-ray tight correlation Gallo et al. 2003)
States of Black Hole Binaries
1 10 100 .01 .1 1 10 100 Energy (keV) Frequency (Hz)
Energy spectra Power density spectra 3.
steep power law compact corona ?
G > 2.4;
rms
< 0.15 ;
f
disk < 80% + QPOs (or
f
disk < 50%)
Neutron stars (atoll type) have thermal and hard states, but they never show strong SPL spectra!
Hard State of BHBs
mechanism? geometry?
• •
Hybrid models: Synchrotron/Compton
(Markoff, Nowak, & Wilms 2005) Kalemci et al. 2005
ADAF-fed Syn./Comp.?
(Yuan, Cui, & Narayan 2005)
Cause of jets?
(GRMHD?) Vertical, external
B
can amplify modest outflows of standard sims.
XTEJ1118+480 (low N H )….truncated, cool disk (McClintock et al. 2001)
Steep Power Law
BHB Gamma Ray Bright State (Grove et al. 1998)
blackbody energetics SPL |
Physical Models for BHB States
Energy spectra Power density spectra State
steep power law physical picture Disk + ??
thermal
hard state
Energy (keV) Frequency (Hz)
3 X-ray States
3 Different Accretion Systems?
Energy spectra YES!
Statistical Distributions in key parameters YES!
6 BHBs [417 thermal; 214 hard; 184 SPL; 179 INT (all types)] GRO J1655-40 (1996-97) XTEJ1550-564 (4 outbursts) XTE J1859+226 (1999-2000) GX339-4 (3 outbursts) 4U1543-47 (2002) H1743-322 (2003)
Power law : thermal (disk) coupling YES!
Distributions in Photon Index
Hard SPL Thermal
Distributions in Temperature
Hard Thermal SPL
Distributions in Disk Fraction (2-20 keV)
Hard SPL Thermal
“Unified Model for Jets in BH Binaries” Fender, Belloni, & Gallo 2004 Remillard 2005
Coupling: power-law and thermal components
GRO J1655-40 XTE J1859+226 XTE J1550-564 Hard: cannot see disk Thermal : yes SPL : no
Conclusions
Observations of BH X-ray states : need 3 models !
Thermal state: weakly magnetized disk (GR/MCD + MRI) seems quite satisfactory Hard state: key topics: hot flow : jet coupling ; spin?
SPL state : PL:disk flux uncoupled; non-thermal corona (to MeV?); LFQPOs ; HFQPOs ; kinship to hard state is a key question
GR in SPL State: High Frequency QPOs
High Frequency QPOs
source HFQPO n (Hz) GRO J1655-40 300, 450 XTE J1550-564 GRS 1915+105 184, 276 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 ------ ISCO for 10 M o BH: n f = 220 Hz (a * = 0.0) Condensations at preferred radii QPOs (Schnittman & Bertschinger 2004) 728 Hz (a * = 0.9)
High Frequency QPOs
source HFQPO n (Hz) GRO J1655-40
300, 450
XTE J1550-564 GRS 1915+105
184, 276
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
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)
Torus Models
(Rezzolla et al. 2003; Fragile et al. 2005) GR ray tracing of accretion torus (Bursa et al.)
Other Models
(disk magnetosphere effects: Li & Narayan 2004 ; Alfven waves: Zhang et al. 2004)
HFQPO Frequencies vs. BH Mass
GROJ1655, XTEJ1550, and GRS1915+105
n
qpo at 2
n
o :
n
o = 931 Hz / M x
Same QPO mechanism and similar value of a * Compare subclasses while model efforts continue
LFQPO Subtypes
XTEJ1550-564
Wijnands et al. 1999 Cui et al. 1999 Remillard et al. 2002 Rodriguez et al. 2004 Casella et al. 2005 Type: Phase Lag: n 0 (Hz):
a
(rms %)
Q
: State: HFQPO coupling
A
soft
B
hard ~8 ~6 few 2 – 3 SPL yes, 3 n o few ~10 SPL yes, 2 n o
C
near zero 0.1 – 15 5 – 20 ~10 Hard/Int.
no HFQPOs
QPOs across states Jet
INT
SPL ?? diff. mechanism ?? evolution in magnetic instability