High Resolution Spectra of Accretion Disk Winds John Raymond What parameters can you derive? Mass . M accretion . M wind Router Mukai et al. 2003 Rinner Spin Inclination Magnetic geometry Mauche 2004 SS Cyg DIAGNOSTICS Emission or Absorption Lines Ionization Parameter or Temperature Recombination Collisional Ionization Time-Dependent Ionization Column Density Density O V K Line Profiles Velocity Velocity Width EX Hya? P Cygni Abundances Kaastra et al. 2005 DIAGNOSTICS II Emission or Absorption Lines Ionization Parameter or Temperature Recombination Collisional Ionization Time-Dependent Ionization Liedahl et al. Paerels et al Cyg X-3 What Physics can you investigate? Heating (dissipation) Turbulence Boundary Layer Disk ADAF or ADIOS Photoionization Winds (Warm Absorbers) Radiation Pressure Thermal Pressure Magnetic driving (Blandford & Payne or small scale fields) . . Significance of M and E Jimenez-Garate et al Accretion Disk Winds . High M CVs -- ~ 3000 km/s -- low. ionization state: <QNe>~5 . -- Mwind ~ 0.1 Macc -- modest collimation -- from or near boundary layer AGN -- ~ 1000 km/s -- Range of ionization states: QFe = 7-24 . . -- Mwind . = 0.02 to 0.05 Macc . -- originate 0.01 to 1 pc from BH, ~103 to 104 Rs -- clumpy, multiphase LMXBs -- 1000 km/s -- high ionization QFe ~ 22 - 27 -- Mwind up to Macc. . 10 -- ~ 10 cm 103 Rs --- narrow range of ionization parameter Jimenez-Garate et al. 2005 Her X-1 Low State Illuminated accretion disk Lines washed out when central source is visible Agrees with reprocessing domination in optical Evaporation or Condensation Jimenez-Garate et al. 2001 Lines From Winds OY Car Outburst; Mauche & Raymond 1000s of km/s Biconical Flows P Cygni profiles Pure scattering lines (Only resonance lines seen) Cir X-1; Schulz & Brandt Cal 87; Greiner et al. AGN Absorption Lines Range of Ionization States O III = O VIII Fe M and L shell Ions (Unlike most X-ray binaries) Very good agreement between model and observations (Instrumental artifacts Limitations of atomic data) Unresolved Transition Arrays Chelouche & Netzer 2005: NGC 3783 AGN Absorption Lines Strong 1000 km/s Wind Finite radial extent Moderate Ionization Radiation Pressure, Thermal Pressure Adiabatic Cooling Multiphase Medium Chelouche & Netzer Krongold et al. 2007: NGC 4151 GRO1655-40 April 1, 2005 90 Absorption Lines! (2 is typical) Constant for 64 ksec Lines of Na, Al, P, Cl, K, Ti, Cr, Mn, Co Fe XXII – XXVI Fe XXIV 2-3 to 2-10 Density sensitive ratios 300-1600 km/s Blue-shifts WIND 3x1037 erg/s Very Soft Miller et al. 2006 Miller et al. VERY Highly Ionized compared to AGN Need to use Voigt profiles to model EW (saturation) High A values mean little flat part to curve of growth Double Abundances of O, Ne and Ca-Ni to match (Does not agree with optical abundances of Israelian et al. or González Hernández et al. enhancement of Si and S) Low Covering Factor: > 6° (no eclipse) < 12° (no Fe XXIV 3s-2p) Fe XXII ne determines fine structure populations of 2p level (Mauche et al.) 2s2p4p 2P 2s2 4d 2D 3/2 , 2D 5/2 2s2p3p 2P 2s2 3d 2D 3/2 , 2D 5/2 2s2 2p 2P 1/2, 2P 3/2 11.77 and 11.92 Å lines Radiation Negligible Not Saturated Radiative Driving? Opacity in UV Lines O stars, CVs?, AGN NO: Add up force in lines High Ionization-no UV Lines Force Multiplier=1.6 Thermal Driving Compton Heating Photoionization heating Begelman et al. Magnetic Processes Magneto-centifugal Poynting Flux from MRI Blandford/Payne; Miller/Stone Thermally Driven Wind? Woods et al. Begelman, McKee & Shields TIC = 1.4x107 K RIC= 10 11.7 cm (cs=vesc) Wind at r > 0.1 to 0.2 RIC r > 10 10.7 cm Woods et al. Full heating, cooling and hydro Illuminating spectrum very similar to GRO1655-40 Proga & Kallman Disk UV can help launch wind, but density still low Where is the gas in GRO1655-40? ξ = L/nr2 N = nr = L/ξr r < L/Nξ (L from continuum, N and ξ from lines) OR r = (L/nξ)1/2 (n from Fe XXII) Miller et al. 2006: r < 10 9.5 cm < 0.01 RIC Netzer 2006 : r0 = 10 10.7 cm Miller et al. 2007: r0 < 10 10 cm < 0.02 RIC Slab vs 1/r2 : Not Thermally Driven : Maybe Thermally Driven : Not Thermally Driven (allows somewhat lower ) Fe XXII density ( 11.77Å line cannot be saturated given 2p-4d lines) Woods et al Mass Loss Rate . M = vA Woods et al predict a peak mass loss rate of 6x10–6 g/(cm2 s) (scaled with BH mass) Divide by v=500 km/s (Vertical wind makes it worse.) nmax = 1011 cm-3 vs observed 1014.6 cm -3 THERMAL WIND PREDICTS A DENSITY TOO LOW BY ORDERS OF MAGNITUDE equatorial Magnetic Disk Wind Model Proga 2003 Equatorial Matches modest solid angle v = few*10^(2-3) km/s Few hundred km/s Matches observed Doppler shift high m-dot High M-dot Matches High density Thermally driven wind may explain more typical high , low ne when only Fe XXV and Fe XXVI are detected? Conclusions Disks and Winds give rich absorption and emission spectra with lots of diagnostic possibilities. Emission lines are visible when central continuum is obscured. Disk emission from LMXRBs is consistent with a photoionization dominated corona. Winds are ubiquitous is CVs, AGN and XRBs. Mass loss rates are significant compared to accretion rates. Radiation pressure is not sufficient. Thermal pressure may be sufficient for AGNs and some XRB spectra, but not for the GRO1655-40 low soft state or for CVs in the high state. Therefore, magnetic forces are important in some cases. Extra Slides Netzer argued Fe XXII 11.77Å line is saturated, but patchy to allow n2/n1 ~ 0.1 Identified 11.54Å and 11.42Å as weaker Fe XXII lines, but Separation is wrong and 11.42 is too strong. 2p – 4d 2s – 4p? Predicts 8.97 Å 2p 2P1/2 - 4d line stronger than 11.92Å 2p 2P3/2 – 3d line. Fails by more than a factor of 4. Nearly optically thin ratio matches prediction. 2.6mÅ : 16 mÅ Model Ingredients/Constraints Photoionized gas Ionizing spectrum Density structure (Slab, wind, hydrostatic) Velocity structure Abundances Radiative Transfer Lots of Atomic Physics CLOUDY, XSTAR, ION Hot Plasma Temperature structure (ADAF, BOUNDARY LAYER) Density structure Velocity Structure Abundances Lots of Atomic Physics APEC, MEKAL, CHIANTI