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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 (10 35 > L x > 10 39 erg/s) Frequent, Rapid Transitions ; Distinct Spectral and Timing Properties

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The X-ray States and High Frequency Oscillations of Black Holes Binaries

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  1. The X-ray States and High Frequency Oscillations of Black Holes Binaries Ron Remillard, MIT Primary Collaborator, Jeff McClintock CfA

  2. 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

  3. 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

  4. BH Outbursts & States X-ray states: Thermal x Hard (jet)g Steep Power Law D Intermediate O

  5. Thermal State Energy spectraPower density spectraStateDefinition accretion disk disk emits > 75% of energy thermalpower continuum: rms < 0.06no QPO with rms > 0.005 weak power continuum ______ | | weak power law

  6. Hard State Energy spectraPower density spectraStateDefinition thermal disk energy fraction < 0.2 hard state power law spectrum: G1 < 2.1 power continuum rms > 0.1 Broken power law G1G2 |______| strong power continuum Fe line

  7. Steep Power Law State Energy spectraPower density spectraStateDefinition power law G > 2.4 steep power law disk fraction < 0.8 QPO (0.1 – 30 Hz) continuum rms < 0.075 thermal hard state Steep power law Quasi-Periodic Oscillations Hz: 11 184 | | disk Fe

  8. Physical Models for BHB States Energy spectraPower density spectraStatePhysical Model Disk + ?? steep power law thermal hard state

  9. X-ray States: The Movie

  10. X-ray States: The Movie

  11. States of Black Hole Binaries Sources “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 J1650-500 GRO J1655-40 GX339-4 H1743-322 (gaps between state parameters [4] SL 1746-331 are more frequently occupied XTE J1748-288 in “problem” sources) XTE J1817-330 XTE J1818-245 XTE J1859+226 XTE J2012+381

  12. Unified Model for Jets in BH Binaries Fender, Belloni, & Gallo 2004 Remillard 2005 Thermal x Hard (jet)g Steep Power Law D Intermediate O Hard Color

  13. BH States: Overview Plots GRO J1655-40 1996-97 outburst Thermal x Hard (jet)g Steep Power Law D Intermediate O

  14. BH States Overview H1743-322 Mxunknown (ISM dust) HEAO-1 outburst: 1977 RXTE: 2003; smaller 2005 + 5 faint ones 2006-2009 Thermal x Hard (jet)g Steep Power Law D Intermediate O

  15. BH States Overview 4U1543-47 Mx = 10 + 1.2 Mo Outbursts 2002 Thermal x Hard (jet)g Steep Power Law D Intermediate O

  16. BH States Overview XTE J1859+226 Mx = + 1.2 Mo Outburst 1999 Thermal x Hard (jet)g Steep Power Law D Intermediate O

  17. BH States Overview XTEJ1550-564 Mx = 9.6 + 1.2 Mo Outburst 1998 ; smaller, 2000; + 3 faint hard-state outbursts 2001, 2002, 2003 Thermal x Hard (jet)g Steep Power Law D Intermediate O

  18. Short-cut to Sates Classification? 80-90% success in regions of plane: Normalized hard color vs. 1-s flickering

  19. 3-State Prescription vs. Hard/Soft States • 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

  20. 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?

  21. High Frequency QPOs (100-450 Hz) 8 Black Hole Binaries with transient HFQPOs 4 with two QPOs (seldom at the same time) 4 seen solo several require multiple observations to gain a single detection

  22. Preferred HFQPO Frequencies HFQPO stability Variable n ? constant to 5% outliers can shift 15% n correlation 3:2 ratio X-ray state Steep Power Law Luminosity range factors ~ 3-6

  23. 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 -------

  24. 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

  25. HFQPO Frequencies vs. BH Mass no = 931 Hz / Mx • Same QPO mechanism and similar spin • Compare subclasses while model efforts continue

  26. 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)

  27. 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}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)

  28. HFQPOs and States: GROJ1655-40 (1996) 300 Hz only ; 7-30 keV both HFQPOs 450 Hz only ; 15-30 keV

  29. Dynamical Frequencies in General Relativity • nf“Keplerian” frequency

  30. Dynamical Frequencies in General Relativity • nqpolar angle • frequency

  31. Dynamical Frequencies in General Relativity • nr radial frequency ISCO Innermost Stable Circular Orbit

  32. Disk Radiation in General Relativity Radius of peak emissivity Page & Thorne 1974

  33. QPO Frequencies High-frequency QPOs

  34. QPO Frequencies \ High-frequency QPOs

  35. QPO Frequencies QPOs:168 113 Hz 67

  36. 67 Hz Detections in GRS1915+105 28 detections > 4 s ; stable to 2 Hz over 12 years

  37. 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 Rgand 3:2 frequency ratio • MHD simulations: what seed conditions  strongly magnetized disk? Steep power law spectrum (and HFQPOs) need your attention !

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