correlations between spectral and lfqpo timing parameters
DESCRIPTION
Correlations Between Spectral and LFQPO Timing Parameters. Summary of draft results prepared by Jeff McClintock for MIT Workshop on Magnetized Accretion Disks Based on work by J. McClintock, R. Remillard, M. Rupen A. Levine, C. Bailyn, J. Orosz, V. Dhawan, G. Pooley October 19, 2006. - PowerPoint PPT PresentationTRANSCRIPT
Correlations Between Spectral and LFQPO Timing Parameters
Comparison of H1743-322 and XTE J1550-564
Summary of draft results prepared by Jeff McClintock for MIT Workshop on Magnetized Accretion Disks
Based on work by J. McClintock, R. Remillard, M. RupenA. Levine, C. Bailyn, J. Orosz, V. Dhawan, G. Pooley
October 19, 2006
Introductory Comments• Numerous spectral/timing correlations exist
• Featured here are remarkably similar correlations observed for H1743-322 and XTE J1550-564
• Results based on diskbb+PL & RXTE/PCA data
• XTE J1550-564: Sobczak et al. (1999) and Remillard et al. (2002)
• H1743-322 results from McClintock, Remillard, Rupen et al. (2007)
• Large literature on correlations ignored: e.g., Markwardt et al. 1999; Muno et al. 1999; Revnivtsev et al. 2000; Sobczak et al.
2000; Titarchuk & Fiorito 2004; Titarchuk & Shaposhnikov 2005
Key to Outburst States of BHs
• Hard (H): blue squares
• Intermediate (INT = H:SPL): yellow circles or magenta circles
• Steep Power Law (SPL): green triangles
• Thermal Dominant (TD): red crosses
0 100 200 Day Number
0 100 200 Day Number
Mod
el F
lux
(1e
-8 c
gs)
0
5
10
15
M
odel
Flu
x (1
e-8
cg
s)
0
1
2
3
4
5
RXTE Pointed Obs.2 – 20 keV Unabsorbed
SPL
SPL
TD
TD
H
H
INT
INT
H1743-322 (2003)
XTE J1550-564 (1998-1999)
X-ray Light Curves
XTE J1550-564: First 40 Days
0 100 200 Day Number
Mod
el F
lux
(1e
-8 c
gs)
0
5
10
15
7 Crab flare (not shown)
H1743-322: First 65 Days
0 100 200 Day Number
Mod
el F
lux
(1e
-8 c
gs)
0
1
2
3
4
5
QPO Frequency vs. Disk Flux
MagnifiedFull range
~20% Lmax
Linear Disk-Flux / Frequency Correlation
accretion disk regulates QPO frequency
• But, QPOs tied to PL (~20-40% PL flux to trigger)
• Further, spectrum of QPOs hard PL
• PL flux strongly dominates over disk flux
• QPO rms power can exceed what the disk can supply
QPO Frequency vs. Photon Index
Onset of linear regimeHard state: index ~ 1.5
Freq. ~ 0.2 HzRin ~ 500 Rg
kT ~ 0.1 keV
End of linear regimeSPL state: index ~ 2.7
Freq. ~ 6 HzRin ~ 50 Rg
kT = 0.5-1 keV
However, Disk too hot for Rin ~ 50 Rg
Unknown QPO mechanismEtc.
QPO Frequency vs. Amplitude QPO Frequency vs. rms Power
Power Density (0.1 – 1 Hz) vs. Disk Flux
Conclusions
• Wide array of spectral/temporal correlations
• H1743-322 and XTE J1550-564 show remarkably similar correlations
• Most striking is the correlation of QPO freq. with disk flux for L < ~20% LEdd and freq. < 6 Hz
• Second key correlation: QPO freq. with PL index
L ~ 20% Lmax