Probing Accretion and Spacetime with Black Hole Binaries

1. Probing Accretion and Spacetime with Black Hole Binaries Shane DavisIAS Omer BlaesIvan HubenyNeal TurnerJulian KrolikJim StoneShigenobu Hirose Chris DoneMathew MiddletonMarek GierlinskiRebbeca ShafeeRamesh NarayanJeff McClintockRon RemillairdLi-Xin Li

2. Issues Addressed in This Talk • How does the release of gravitational binding energy lead to thermal radiation? • Are thin disk (-disk) models sufficient to explain black hole X-ray binary (BHB) observations?

3. The thin disk model • H/R << 1 • Constant accretion rate; time-steady • Gravitational binding energy released locally as radiation: The -disk model • determines surface density  • Vertical dissipation distribution:

4. The Multicolor Disk Model (MCD) • Assumes simple temperature distribution: • Spectrum assumed to be color-corrected blackbody: F  F 

5. Disk Dominated Spectra LMC X-3 • L prop. to T4 suggests fcol and emitting area are constant Gierlinski & Done 2004

6. Comparison with Previous Spectral Models • Previous -disk models provide mixed results • Shimura & Takahara (1995); full atmosphere calculation, free-free emission and Compton scattering: stars • Merloni, Fabian & Ross (2000); relativistic effects, constant density, f-f emission and Compton scattering: blue curve • Small scatter in L-T relation as L varies by over an order of magnitude Gierlinski & Done 2004

7. Our Models, Briefly • Use conservation laws with Kerr metric to calculate one-zone model • Full disk model is determined by ~4 parameters: M, a/M, L/LEdd,  • Calculate self-consistent vertical structure and radiative transfer in a series of concentric annuli • Each annulus is determined by 3 parameters (+ assumptions): Teff, Q, (g=Q z),  • Calculate photon geodesics in a relativistic spacetime (ray tracing) -- determined by a/M and i

8. Model Parameters L/LEdd Inclination Spin Mass

9. Luminosity vs. Temperature • We generate artificial spectra and fit MCD model • Then, we follow the procedure of Gierlinski & Done (2004) to calculate Ldisk/Ledd and Tmax • Model: a=0, i=70o, M=10 solar masses, and =0.01

10. Spin Estimates • With independent estimates for the inclination, mass, and distance, thermal component only has two free parameters -- luminosity and spin (same number as diskbb) • Fits with our models suggest moderate (a/M < 0.9) values for several sources Shafee et al. 2005

11. ‘Broadband’ Fits to LMC X-3 Our Model MCD • MCD model is too narrow -- need relativistic broadening 2 ~ 100 • Best fit find spinning black hole with a/M=0.27

12. What Have We Learned? • Our detailed accretion disk models can reproduce the spectra of disk dominated BHBs (statistically significant improvement over MCD for ‘broad-band’ spectra of LMC X-3) • Models qualitatively reproduce the observed evolution with luminosity; spectral modeling may constrain the nature of angular momentum transport (i.e. measure ) and black hole spin What Have I Skipped? • Dissipation, magnetic stresses, inhomogeneities, etc. can affect the spectra -- more progress is needed to make these methods more robust

13. Luminosity vs. Temperature • Slight hardening is consistent with some observations • Allows one to constrain surface density and accretion stress • Models become effectively optically thin at high accretion rates =0.1 =0.01 =0.001

14. Summary of Fit Results a*~0 =0.01 a*~0.1 =0.01 a*~0.65 =0.1

15. II. Adding ‘Real’ Physics: Dissipation, Magnetic Stresses & Inhomogeneities

16. Local MRI Simulations(with radiaton) • Shakura & Sunyaev (1973): • Turner (2004): Mass more centrally concentrated towards midplane in simulations. • Magnetic fields produced near midplane are buoyant and dissipate near surface Turner (2004)

17. Dissipation Profile • Modified dissipation profile changes structure significantly • Where -dF/dm is small (large), density is larger (smaller) • Note that T and  near * are similar Turner Profile SS73 Profile

18. Dissipation Profile • … but modified dissipation profile has limited affect on the spectrum. • This particular annulus is very effectively optically thick and *is close to surface Turner Profile SS73 Profile

19. Dissipation Profile • Consider same dissipation profile, but in an annulus that is not effectively optically thick. • Spectrum with modified dissipation profile is effectively optically thick, but has a much greater surface temperature Turner Profile SS73 Profile

20. Dissipation Profile • For this annulus, the spectra from the modified dissipation profile is considerably harder • This will exacerbate the discrepancy between observations and models unless disks stay optically thick Turner Profile SS73 Profile

21. Black Hole Accretion Disk Spectral Formation

22. Spectral Formation • Depth of formation *: optical depth where (esabs)1/2~1  > *: absorbed  < *: escape • Therefore Thomson scattering produces modified blackbody: • Compton scattering gives softer Wien spectrum which Shimura & Takahara claim is consistent with fcol~1.7 for BHBs = 0 es= 1 (es abs)1/2= 1 abs= 1

23. How can we improve on these models? • Include metals with bound-free opacity; solve non-LTE populations • More accurate radiative transfer and better treatment of Compton Scattering • Can consider the effects of more complicated physics: e.g. dissipation, magnetic stresses, and inhomogeneities

24. Magnetic Stresses • B2/8 & dF/dm taken from simulations of Hirose et al. • Gas pressure dominated -- dF/dm has little effect on the structure • Extra magnetic pressure support lengthens scale height hr • *~*/(es hr) No B field B field Simulation

25. Magnetic Stresses • Lower * and higher T* combine to give somewhat harder spectrum • In this case lower * alters statistical equilibrium -- lower recombination rate relative to photoionization rate give more highly ionized matter with lower bound-free opacity No B field B field

26. Inhomogeneities • Radiation pressure dominated accretion disks expected to be homogeneous due to photon bubble instability and/or compressible MRI • May make disk thinner and (therefore) denser (Begelman 2001, Turner et al. 2005) • May also affect the radiative transfer… Neal Turner

27. Inhomogeneities • 2-D Monte Carlo calculations: photon bubbles help thermalize the spectrum, making it softer • Photon emission and absorption dominated by denser regions.

28. Non-aligned Jet • XTE J1550-564 is a microquasar • Hannikainen et al. (2001) observe superluminal ejections with v > 2 c • Ballistic model: • Orosz et al. (2002) found i=72o • Non-aligned jets not uncommon -- usually assumed that BH spin differs from binary orbit and inner disk aligns with BH -- Bardeen-Petterson effect • Best fit inclination, spin: i=43o, a*=0.44

29. Spectral States of BHBs • Spectral states specified by relative contributions of thermal (disk) and non-thermal emission (corona) • High/Soft state is dominated by thermal disk-like component Done & Gierlinski 2004

30. Spectral Dependence on Surface Density • Spectra largely independent of for large surface density (>~ 103 g/cm2) • As disk becomes marginally effectively thin, spectra become sensitive to  and harden rapidly with decreasing 

31. Binaries Provide Independent Constraints on Models • Orosz and collaborators derive reasonably precise estimates from modeling the light curve of secondary • e.g. XTE J1550-564:

32. Luminosity vs. Temperature • Measured binary properties limit parameter space of fits • Simultaneous fits to multiple observations of same source constrain spin/torque • Spectra are too soft to allow for extreme spin/large torques

33. Stellar Atmospheres: Disk Annuli vs. Stellar Envelopes • The spectra of stars are determined by Teff, g, and the composition • Annuli are determined by, Teff, Q (where g=Q z), , the composition, and the vertical dissipation profile: F(m) • Teff, Q, and  can be derived from radial disk structure equations • Standard assumption is:

34. Luminosity vs. Temperature Gierlinski & Done 2004

35. Effect of bound-free opacity • Bound-free opacity decreases depth of formation:  • Absorption opacity approximately grey • Spectrum still approximated by diluted blackbody:

36. The Multicolor Disk Model (MCD) • Consider simplest temperature distribution: • Assume blackbody and integrate over R replacing R with T (Tmax~fcolTeff):

37. Effective Temperature: Teff

38. Gravity Parameter: Q

39. Comparison Between Interpolation and Exact Models • Interpolation best at high L/Ledd • Exact: Blue curve Interpolation: Red Curve