Pinhole Cam Visualisations of Accretion Disks around Kerr BH

Transcription

1 Pinhole Camera Visualisations of Accretion Disks around Kerr Black Holes March 22nd, 2016

2 Contents 1 General relativity Einstein equations and equations of motion 2 Tetrads Defining the pinhole camera Defining the accretion disk 3 Intensity, redshift and coordinate patches Code validation Movies of different orbits 4

3 The Einstein equations Einstein equations and equations of motion The metric tensor is determined by the Einstein equations: G µ ν + g µ νλ = 8πT µ ν. (1) In vacuum on small scales they reduce to R µ ν = 0. (2)

4 Schwarzschild and Kerr spacetime Axisymmetric stationary Kerr spacetime: where ds 2 = ( 1 2Mr Σ 2 ) dt 2 4Mar Σ 2 Einstein equations and equations of motion sin 2 θ dt dφ + Σ2 dr 2 + Σ 2 dθ 2 + A Σ 2 sin2 θ dφ 2, (3) Σ 2 = r 2 + a 2 cos 2 θ, (4) = r 2 2Mr + a 2, (5) ( A = r 2 + a 2) 2 a 2 sin 2 θ. (6)

5 Horizons Einstein equations and equations of motion [Bardeen 1972, Visser 2008, Younsi 2013]: red: static limit (r 0 ) dark-blue: outer event horizon (r + ) green: inner event horizon (r ) turquoise: inner static limit ( r ) only physical singularity at: Σ 2 := r 2 + a 2 cos 2 θ = 0.

6 Einstein equations and equations of motion Geodesic equations in Boyer-Lindquist coordinates Using 2L = g µν ẋ µ ẋ ν (Lagrangian of a freely falling test particle) one obtains the following equations for geodesics in Kerr spacetime [Younsi 2013]: ṫ = E + 2Mr [ ( Σ 2 r 2 + a 2) ] E al z, (7) ṙ 2 = (µ Σ 2 + Eṫ l z φ Σ 2 θ 2), (8) θ 2 = 1 ( ) ] [Q Σ 4 + E 2 + µ a 2 cos 2 θ lz 2 cot 2 θ, (9) ( ) φ = 2aMrE + Σ 2 2Mr l z csc 2 θ Σ 2. (10)

7 Einstein equations and equations of motion Geodesic equations in Boyer-Lindquist coordinates Move to second derivatives of r and θ to avoid the squares. 6 coupled differential equations (ṫ, ṙ, r, φ, θ, θ). Solved by fourth order Runge-Kutta with fifth order Runge-Kutta error precision control.

8 Tetrads Defining the pinhole camera Defining the accretion disk Image-plane method vs. pinhole camera method

9 Pinhole camera method Tetrads Defining the pinhole camera Defining the accretion disk

10 What are tetrads? Tetrads Defining the pinhole camera Defining the accretion disk A tetrad is a set of orthonormal basis vectors [Misner et al. 1973] e (ˆµ) e (ˆν) = ηˆµˆν. (11) Counter-example: Basis vectors in Boyer-Lindquist coordinates are neither normalised, nor orthogonal to each other: e (µ) e (ν) = g αβ e α (µ) eβ (ν) = g αβδ µ α δ ν β = g µν. (12)

11 Tetrads Defining the pinhole camera Defining the accretion disk Constructing a stationary observer s tetrad Define the pinhole camera s four-velocity as e (ˆt) := (u µ ) = ( u t (x µ ) o ) = e t (ˆt) et (t), (13) where it was used that e t (ˆt) = ut [Misner et al. 1973]. This yields: 1! = e (ˆt) e (ˆt) = ( e t (ˆt)) 2 e(t) e (t) (14) e t (ˆt) = 1 gtt e t (t) (15)

12 Tetrads Defining the pinhole camera Defining the accretion disk Constructing a stationary observer s tetrad Similarly suitable ˆθ and ˆr vectors are obtained: e (ˆr) = 1 e (r) = grr Σ e (r), (16) e (ˆθ) = 1 gθθ e (θ) = 1 Σ e (θ). (17) The ansatz for the φ-basis vector must respect the off-diagonal terms of the Kerr metric in BL coordinates: e ( ˆφ) = K ( x i) ( e (φ) + P x i) e (t). (18)

13 Tetrads Defining the pinhole camera Defining the accretion disk Constructing a stationary observer s tetrad The orthonormality conditions give two equations, which are used to determine K and P. This finally yields: e ( ˆφ) = ( gtt e (φ) g ) φt e sin θ g (t) tt. (19)

14 Initialising the four-momenta Tetrads Defining the pinhole camera Defining the accretion disk Pinhole camera method by Bohn et al. (2014): ξ µ = C e µ (ˆt) eµ (ˆr) β r 0 e µ (ˆθ) α r 0 e µ ( ˆφ) (20) C normalisation constant, which is determined by p p = µ (µ = 0 for photons and µ = 1 for massive particles). r 0 causes that the pinhole camera zooms in on the accretion disk. α, β are spaced equidistant in the interval [ 22M, 22M].

15 Angular velocity profile Tetrads Defining the pinhole camera Defining the accretion disk assume fast rotating disk, trajectories of emitters approximated by circular motion [cf. Shakura and Sunyaev 1973] inner edge of disk at ISCO: r inner = r ISCO ; outer edge: r outer = 20M. Particles on circular orbits in the equatorial plane have an angular velocity of [Bardeen et al. 1972] dφ dt = Ω K = M a. (21) M + r 3/2

16 Redshift Tetrads Defining the pinhole camera Defining the accretion disk Define fluid s and observer s four-velocity: ( ) u µ fluid = (ufluid, t 0, 0, u φ fluid ) = ufluid(1, t 0, 0, Ω K ), (22) ( ) u µ obs = (uobs, t 0, 0, 0). (23) Using E fluid = p α ufluid α one obtains: g = 1 + z := E fluid E obs = ṫfluid ṫ obs ( 1 Ω K l z E ) (24) [Courtesy of Dr. Younsi, who kindly gave me this derivation].

17 Tetrads Defining the pinhole camera Defining the accretion disk General relativistic radiative transfer (GRRT) equations Computation of intensity by solution of the GRRT equations [Fuerst and Wu 2004, Baschek et al. 1997]: ( di dλ = p αu α λ α 0,ν I + j ) 0,ν ν0 3. (25) Equivalent formulation [Younsi 2013]: dτ ν dλ = gα 0,ν, (26) ( ) di dλ = g j0,ν e τν. (27) ν 3 0

18 Tetrads Defining the pinhole camera Defining the accretion disk Lorentz-invariant intensity [Rybicki and Lightman 2004, Younsi 2013]: I = I ν /ν 3 ; specific intensity: I ν optical depth [Baschek et al. 1997, Younsi 2013]: τ ν (λ) = λ λ 0 α 0,ν (λ )p α u α λ dλ, where α ν is the absorption, defined by [Rybicki and Lightman 2004] di ν = α ν I ν ds, with the distance ds the beam travels assumed vanishing absorption outside the disk: α 0,ν! = 0 ansatz for the emissivity coefficient: j 0,ν r 3.

19 Code structure Tetrads Defining the pinhole camera Defining the accretion disk Makeimage setup α and β Integration Geodesic ICs Iλi, λi+1 = λi + λ Runge-Kutta p µ 0, E, lz, Q GRRT-solver False photon intersected, captured, or escaped True Termination

20 Redshift (r, θ) = (1000 M, 85 ) Intensity, redshift and coordinate patches Code validation Movies of different orbits left: a/m = 0, right: a/m = 0.998

21 Higher order photons Intensity, redshift and coordinate patches Code validation Movies of different orbits Higher order photons can make several turns around the black hole. This yields the characteristic photon rings.

22 Intensity (r, θ) = (1000 M, 85 ) Intensity, redshift and coordinate patches Code validation Movies of different orbits left: a/m = 0, right: a/m = 0.998

23 Intensity, redshift and coordinate patches Code validation Movies of different orbits Inner most stable circular orbit (ISCO) [Bardeen 1972] Green line for counterblue line for co-rotating (massive) particles. In the Schwarzschild limit the ISCO for co-rotating particles coincides with the ISCO of counter-rotating ones.

24 Rotation in θ animation, a/m = 0.5 Intensity, redshift and coordinate patches Code validation Movies of different orbits

25 Intensity, redshift and coordinate patches Code validation Movies of different orbits Coordinate patches (r, θ) = (1000M, 25 ) left: a/m = 0, right: a/m = 0.998

26 Intensity, redshift and coordinate patches Code validation Movies of different orbits Coordinate patches (r, θ) = (1000M, 85 ) left: a/m = 0, right: a/m = 0.998

27 Intensity, redshift and coordinate patches Code validation Movies of different orbits Coordinate patches (r, θ) = (5M, 85 ) left: a/m = 0, right: a/m = 0.998

28 Up-spinning black hole Intensity, redshift and coordinate patches Code validation Movies of different orbits

29 Intensity, redshift and coordinate patches Code validation Movies of different orbits Comparison of 1 + z left: r = 10 3 M, right: r = 10 6 M a/m = 0.998, θ = 85

30 Hyperbolic Orbit a/m = 0.5 Intensity, redshift and coordinate patches Code validation Movies of different orbits

31 created a method that is able to visualise the radiation emanating from an accretion flow visualisation tool for curved spacetimes, basically applicable to any other spacetime provides visual description of the GR effects happening close to the horizon (using proper coordinates even below)

32 future work using other disk models/accretion flows implement gravitational lensing of background reconstruction of pinhole camera with comoving tetrad reformulation of code in 3+1 decomposition of spacetime considering other spacetimes, e.g. binary black holes.

33 Thank you for your attention!

34 I J. M. Bardeen, W. H. Press, and S. A. Teukolsky. Rotating Black Holes: Locally Nonrotating Frames, Energy Extraction, and Scalar Synchrotron Radiation. In: Astrophysical Journal 178 (Dec. 1972), pp doi: / B. Baschek et al. Radiative transfer in moving spherical atmospheres. II. Analytical solution for fully relativistic radial motions. In: Astronomy and Astrophysics 317 (Jan. 1997), pp A. Bohn et al. What would a binary black hole merger look like? Version 2. In: (Nov. 2014). arxiv: v2 [gr-qc]. S. V. Fuerst and K. Wu. Radiation transfer of emission lines in curved space-time. In: Astronomy and Astrophysics 424 (Sept. 2004), pp doi: / : eprint: astro-ph/

35 II Charles W. Misner, Kip S. Thorne, and John Archibald Wheeler. Gravitation. W. H. Freeman, isbn: George B. Rybicki and Alan P. Lightman. Radiative Processes in Astrophysics. Weinheim: WILEY-VCH, N. I. Shakura and R. A. Sunyaev. Black holes in binary systems. Observational appearance. In: Astronomy and Astrophysics 24 (1973), pp Matt Visser. The Kerr spacetime: A brief introduction. Version 3. In: (Jan. 2008). arxiv: v3 [gr-qc]. Dr. Ziri Younsi. General Relativistic Radiative Transfer in Black Hole Systems. dissertation. Department of Space and Climate Physics University College London, Oct