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Correlations Between Spectral and LFQPO Timing Parameters

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.

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Correlations Between Spectral and LFQPO Timing Parameters

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  1. 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 Comparison of H1743-322 and XTE J1550-564

  2. 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

  3. Key to Outburst States of BHs • Hard (H): blue squares • Intermediate (INT = H:SPL): yellow circlesormagenta circles • Steep Power Law (SPL): green triangles • Thermal Dominant (TD): red crosses

  4. X-ray Light Curves H1743-322 (2003) SPL Model Flux (1e-8 cgs) 0 1 2 3 4 5 TD RXTE Pointed Obs. 2 – 20 keV Unabsorbed INT H 0 100 200 Day Number SPL XTE J1550-564 (1998-1999) Model Flux (1e-8 cgs) 0 5 10 15 TD INT H 0 100 200 Day Number

  5. XTE J1550-564: First 40 Days 7 Crab flare (not shown) Model Flux (1e-8 cgs) 0 5 10 15 0 100 200 Day Number

  6. H1743-322: First 65 Days Model Flux (1e-8 cgs) 0 1 2 3 4 5 0 100 200 Day Number

  7. QPO Frequency vs. Disk Flux ~20% Lmax Full range Magnified

  8. 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

  9. QPO Frequency vs. Photon Index Onset of linear regime Hard state: index ~ 1.5 Freq. ~ 0.2 Hz Rin ~ 500 Rg kT ~ 0.1 keV End of linear regime SPL state: index ~ 2.7 Freq. ~ 6 Hz Rin ~ 50 Rg kT = 0.5-1 keV However, Disk too hot for Rin ~ 50 Rg Unknown QPO mechanism Etc.

  10. QPO Frequency vs. Amplitude QPO Frequency vs. rms Power

  11. Power Density (0.1 – 1 Hz) vs. Disk Flux

  12. Conclusions L ~ 20% Lmax • 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

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