mit workshop on magnetized accretion disks
DESCRIPTION
This presentation will probably involve audience discussion, which will create action items. Use PowerPoint to keep track of these action items during your presentation In Slide Show, click on the right mouse button Select “Meeting Minder” Select the “Action Items” tab - PowerPoint PPT PresentationTRANSCRIPT
![Page 1: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/1.jpg)
MIT Workshop on Magnetized Accretion Disks
Supported by:MIT-France ProgramCEA Saclay, FranceMIT Kavli Inst. for Astrophysics & Space ResearchMIT Dept. EE&CSRXTE Project
October 19 & 20, 2006
![Page 2: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/2.jpg)
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?
![Page 3: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/3.jpg)
X-ray States of Black Hole Binaries:
Observations and Physical Models
Ron RemillardMIT Kavli Center for Astrophysics and Space Research
![Page 4: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/4.jpg)
Workshop Motivations Assess status of BH accretion physics
General relativity astrophysics at 10 Rg?
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
![Page 5: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/5.jpg)
Active X-ray States of BH Binaries
Thermal State: thermal spectrum ; L T4 ; 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 ??
![Page 6: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/6.jpg)
Black Hole X-ray Nova
GRO J1655-40
First known outbursts: 1994-95;() 1996-97; 2005
Dynamical black hole binary6.3 (0.5) Mo
Relativistic Jets in 1994~Radio-quiet, 1996-97, 2005
![Page 7: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/7.jpg)
Black Hole X-ray Nova
GRO J1655-40
Different X-ray States
![Page 8: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/8.jpg)
Observation Reviews & Global Studies
Done & Gierlinski 2003 MNRAS, 342, 1041
Fender 2006 Compact Stellar X-ray Sources, Ch. 9
Fender & Belloni 2004 ARAA, 42, 317
Charles & Coe 2006 Compact Stellar X-ray Sources, Ch. 5
McClintock & Remillard 2006 Compact Stellar X-ray Sources, Ch. 4
Psaltis 2006 Compact Stellar X-ray Sources, Ch. 1
Remillard & McClintock 2006 ARAA, 44, 49
van der Klis 2006 Compact Stellar X-ray Sources, Ch. 2
Zdziarski & Gierlinski 2004 PThPS, 155, 99
![Page 9: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/9.jpg)
X-ray States of BHBs
1. Thermal State: fdisk > 75%; rms < 0.075 ; no QPOs (amax < 0.5%)
inner accretion disk
![Page 10: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/10.jpg)
X-ray States of BHBs
1. Thermal State:
classical disk model: T(r) ~ r-3/4 L(r) ~ r-2
![Page 11: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/11.jpg)
Heat from Accretion Disk ?
T(r) r-p; p ~ 0.7 (Kubota et al 2005) (GR tweak of p=0.75)
modified disk blackbody
GX339-4 Relativistic Fe line
blackbody energetics GR/Keplerian velocities?
Kubota & Done 2004; Gierlinski & Done 2004
e.g. Miller et al. 2004; butsee Merloni & Fabian 2003
![Page 12: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/12.jpg)
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 = Pgas / (B2/8)
Thermal Radiation from a Weakly Magnetized Disk
Alternatives: low inner disk (external seed B) ?Plasma Rings (Coppi & Rousseau 2006) ?GR MHD: Stronger jets with higher spin ?
Other X-ray states?
![Page 13: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/13.jpg)
Hard State of BHBs
2. Hard State fdisk < 20%; ~ 1.4 - 2.1; rms > 0.10
steady jet (radio emission: collimated, polarized, flat spectrum)
![Page 14: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/14.jpg)
Hard State of BHBs: Steady Radio Jet
2. Hard State fdisk < 20%; ~ 1.4 - 2.1; rms > 0.10
steady jet (radio : X-ray tight correlation Gallo et al. 2003)
![Page 15: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/15.jpg)
States of Black Hole Binaries
3. steep power law
compact corona ?
> 2.4; rms < 0.15 ;
fdisk < 80% + QPOs (or fdisk< 50%)
Energy spectra Power density spectra
1 10 100 .01 .1 1 10 100 Energy (keV) Frequency (Hz)
Neutron stars (atoll type) have thermal and hard states,but they never show strong SPL spectra!
![Page 16: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/16.jpg)
Hard State of BHBsmechanism? 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 amplifymodest outflows of standard sims.
XTEJ1118+480 (low NH)….truncated, cool disk(McClintock et al. 2001)
![Page 17: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/17.jpg)
Steep Power Law
BHB Gamma Ray Bright State(Grove et al. 1998)
blackbody energetics
SPL
|
![Page 18: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/18.jpg)
Physical Models for BHB StatesEnergy spectra Power density spectra
State physical picture
steep power law Disk + ??
thermal
hard state
Energy (keV) Frequency (Hz)
![Page 19: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/19.jpg)
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!
3 X-ray States 3 Different Accretion Systems?
![Page 20: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/20.jpg)
Hard SPL Thermal
Distributions in Photon Index
![Page 21: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/21.jpg)
Hard Thermal SPL
Distributions in Temperature
![Page 22: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/22.jpg)
Hard SPL Thermal
Distributions in Disk Fraction (2-20 keV)
![Page 23: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/23.jpg)
“Unified Model for Jets in BH Binaries”Fender, Belloni, & Gallo 2004 Remillard 2005
![Page 24: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/24.jpg)
GRO J1655-40 XTE J1859+226 XTE J1550-564
Coupling: power-law and thermal components
Hard: cannot see disk Thermal : yes SPL : no
![Page 25: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/25.jpg)
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
![Page 26: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/26.jpg)
GR in SPL State: High Frequency QPOs
![Page 27: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/27.jpg)
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-------
ISCO for 10 Mo BH: = 220 Hz (a* = 0.0) 728 Hz (a* = 0.9)
Condensations at preferred radii QPOs (Schnittman & Bertschinger 2004)
![Page 28: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/28.jpg)
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
![Page 29: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/29.jpg)
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)
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)
![Page 30: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/30.jpg)
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
![Page 31: MIT Workshop on Magnetized Accretion Disks](https://reader035.vdocuments.mx/reader035/viewer/2022081503/56815a73550346895dc7d97f/html5/thumbnails/31.jpg)
LFQPO 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