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Title: Ulrich%20Sperhake


1
Numerical simulations of high-energy
collisions Of black hole
Ulrich Sperhake Friedrich-Schiller Universität
Jena
Work with E.Berti, V.Cardoso, J.A.Gonzalez,
F.Pretorius
Relativity Seminar Austin, 18th March 2008
Work supported by the SFB TR7
2
Overview
  • Black holes in physics
  • General Relativity
  • Ingredients of numerical relativity
  • Results
  • High energy collisions
  • Summary

3
1. Black holes in physics
4
Black Holes predicted by GR
  • Black holes predicted by Einsteins theory of
    relativity
  • Term Black hole by John A. Wheeler 1960s
  • Vacuum solutions with a singularity
  • For a long time mathematical curiosity
  • valuable insight into theory
  • but real objects in the universe?
  • That picture has changed dramatically!

5
How to characterize a black hole?
  • Consider light cones
  • Outgoing, ingoing light
  • Calculate surface area

of outgoing light
  • ExpansionRate of

change of that area
  • Apparent horizon

Outermost surface with zero expansion
  • Light cones tip over due to curvature

6
Black Holes in astrophysics
  • Black holes are important in astrophysics
  • Black holes found at
  • centers of galaxies
  • Structure of galaxies
  • Important sources of
  • electromagnetic radiation
  • Structure formation in
  • the early universe

7
Fundamental physics of black holes
  • Allow for unprecedented tests of fundamental
    physics
  • Strongest sources of Gravitational Waves (GWs)
  • Test alternative theories of gravity
  • No-hair theorem of GR
  • Production in Accelerators

8
Gravitational wave physics
  • Accelerating bodies produce GWs
  • Weber 1960s
  • Bar detector
  • Claimed detection probably not real
  • GWs displace particles
  • GW observatories GEO600, LIGO, TAMA, VIRGO
  • Bar detectors

9
The big picture
Detectors
Physical system
observe
test
Provide info
describes
Help detection
  • Model
  • GR (NR)
  • PN
  • Perturbation theory
  • Alternative Theories?
  • External Physics
  • Astrophysics
  • Fundamental Physics
  • Cosmology

10
2. General relativity
11
The framework General Relativity
  • Curvature generates
  • acceleration

geodesic deviation
No force !!
  • Description of geometry

Metric
Connection
Riemann Tensor
12
The metric defines everything
  • Christoffel connection
  • Covariant derivative
  • Riemann Tensor
  • Geodesic deviation
  • Parallel transport

13
How to get the metric?
  • The metric must obey the Einstein Equations
  • Ricci-Tensor, Einstein-Tensor, Matter tensor

Trace-reversed Ricci
Matter
  • Einstein Equations
  • Take metric
  • Calculate
  • Use that as matter tensor
  • Solutions Easy!
  • Physically meaningful solutions Difficult!

14
The Einstein equations in vacuum
  • Spacetime tells matter how to move,
  • matter tells spacetime how to curve
  • Field equations

Second order PDEs for the metric components
Invariant under coordinate (gauge) transformations
  • System of equations extremely complex Pile
    of paper!

Analytic solutions Minkowski,
Schwarzschild, Kerr,
Robertson-Walker,
Numerical methods necessary for general
scenarios!
15
3. The basics of numerical relativity
16
A list of tasks
  • Target Predict time evolution of BBH in GR
  • Einstein equations
  • Cast as evolution system
  • Choose specific formulation
  • Discretize for Computer
  • Choose coordinate conditions Gauge
  • Fix technical aspects
  • Mesh-refinement / spectral domains
  • Excision
  • Parallelization
  • Find large computer
  • Construct realistic initial data
  • Start evolution and wait
  • Extract physics from the data

Gourgoulhon gr-qc/0703035
17
3.1. The Einstein equations
18
31 decomposition
  • GR Space and time exist together as
    Spacetime
  • Numerical relativity reverse this process!
  • ADM 31 decomposition

Arnowitt, Deser, Misner (1962) York
(1979) Choquet-Bruhat, York (1980)
3-metric
lapse
shift
  • lapse, shift Gauge
  • Einstein equations

6 Evolution equations
4 Constraints
  • Constraints preserved under evolution!

19
The ADM equations
  • Time projection

Hamiltonian constraint
  • Mixed projection

Momentum constraints
  • Spatial projection

Evolution equations
20
The structure of the ADM equations
  • Constraints
  • They do not contain time derivatives
  • They must be satisfied on each slice
  • The Bianchi identities propagate the constraints

If they are satisfied initially, they are always
satisfied
  • Evolution equations
  • Commonly written as first order system
  • Gauge
  • Equations say nothing about lapse and shift
    !

21
The ADM equations as an initial value problem
  • Entwicklungsgleichungen

22
Alternatives to the ADM equations
  • Unfortunately the ADM eqs. do not seem to work
    in NR !!

Weak hyperbolicity Nearby initial data can
diverge
From each other super-exponentially
  • Many alternative formulations have been
    suggested
  • Two successful families so far
  • ADM based formulations BSSN

Shibata Nakamura 95, Baumgarte Shapiro 99
  • Generalized harmonic formulations

Choque-Bruhat 62, Garfinkle 04, Pretorius 05
23
The BSSN equations
24
3.2. Gauge choices
25
The gauge freedom
  • Remember Einstein equations say nothing about
  • Any choice of lapse and shift gives a solution
  • This represents the coordinate freedom of GR
  • Physics do not depend on

So why bother?
  • Avoid coordinate singularities!
  • Stop the code from running into the physical
    singularity
  • No full-proof recipe, but
  • Singularity avoiding slicing
  • Use shift to avoid coordinate stretching

26
3.3. Initial data
27
Initial data problem
Two problems
Constraints, realistic data
  • York-Lichnerowicz split
  • Rearrange degrees of freedom
  • Conformal transverse traceless
  • Physical transverse traceless
  • Thin sandwich

York, Lichnerowicz
OMurchadha, York
Wilson, Mathews York
  • Conformal flatness Kerr is NOT conformally
    flat!

Non-physical GWs problematic for high energy
collisions!
28
2 families of initial data
  • Generalized analytic solutions

Isotropic Schwarzschild
Time-symmetric, -holes
Brill-Lindquist, Misner (1960s)
Spin, Momenta
Bowen, York (1980)
Punctures
Brandt, Brügmann (1997)
  • Excision Data IH boundary conditions on
    excision surface

Meudon group Cook, Pfeiffer Ansorg
  • Quasi-circular
  • Effective potential
  • PN parameters
  • helical Killing Vektor

29
4. Extracting physics
30
Basic assumptions
  • Extracting physics in NR is non-trivial !!
  • Newtonian quantities are not always
    well-defined !!
  • We assume that the ADM variables

Lapse
Shift
3-metric
Extrinsic curvature
are given on each hypersurface
  • Even when using other formulations, the ADM
    variables

are straightforward to calculate
31
Global quantities
  • ADM mass Global energy of the spacetime
  • Total angular momentum of the spacetime

By construction all of these are time-independent
!!
32
Local quantities
  • Often impossible to define !!
  • Isolated horizon framework

Ashtekar and coworkers
  • Calculate apparent horizon
  • irreducible mass, momenta associated with horizon
  • Total BH mass

Christodoulou
  • Binding energy of a binary

33
Gravitational waves
  • Most important result Emitted gravitational
    waves (GWs)
  • Newman-Penrose scalar

Complex 2 free functions
  • GWs allow us to measure
  • Radiated energy
  • Radiated momenta
  • Angular dependence of radiation
  • Predicted strain

34
Angular dependence
  • Waves are normally extracted at fixed radius

are viewed from the source frame !!
  • Decompose angular dependence
  • Modes
  • Spin-weighted spherical harmonics

35
5. Status of black hole simulations
36
A very brief history
  • First attemts Hahn and Lindquist 1960s,
    Eppley and Smarr 1970s
  • Breakthrough Pretorius 2005, Brownsville,
    NASA Goddard 2005
  • Problems
  • Computer resources
  • AMR
  • Instabilities Gauge, Equations
  • Now about 10 codes
  • GHG
  • Moving puncture

37
The BBH breakthrough
  • Simplest configuration
  • GWs circularize orbit
  • quasi-circular initial data

Pretorius 05
  • BBH breakthrough
  • Initial data scalar field
  • Radiated energy

25 50 75 100 4.7 3.2 2.7 2.3
  • Eccentricity

38
Astrophysical binaries basics
  • 4 stages of BBH merger
  • Newtonian inspiral (not GW driven)
  • Post-Newtonian (PN) inspiral phase (GW driven)
  • merger (Numerical Relativity)
  • Ring-down (Perturbation Theory)
  • Free parameters
  • 1 Total mass (merely a scaling factor)
  • 1 Mass ratio
  • 6 Spin
  • 1 Eccentricity GWs circularize orbit
  • NR can only simulate the last orbits

39
Astrophysical binaries Results
  • Equal-mass, non-spinning binaries
  • of the total mass of the system
  • GWs quadrupole dominated
  • Good agreement with PN predictions for GW
    emission
  • Recoil or kick
  • Unequal mass and/or spin kick
  • Certain spin configurations

Enough to eject BHs from galaxies
Observations such large kicks not generic
  • Spin-flip
  • Merger spin realignment
  • X-shaped radio sources

40
Zoom whirl orbits
Pretorius Khurana 07
  • 1-parameter family of initial data linear
    momentum
  • Fine-tune parameter

Threshold of immediate merger
  • Analogue in gedodesics !
  • Reminiscent of

Critical phenomena
41
6. High energy collision
42
Motivation
  • No known mechanism to accelerate BHs to
  • Such collisions unlikely to occur in
    astrophysical scenarios
  • But
  • Probe GR in the most dynamic range
  • Near the speed of light, structure is lost

Collisions might describe generic collisions
  • Test cosmic censorship
  • Threshold of immediate merger Pretorius 2006

Indication of unexpected phenomena
43
Setup of the problem
  • Take two black holes

Total rest mass
Initial position
Linear momentum
  • For now Equal-mass, head-on
  • Target GW energy

Mode distribution of GW energy
44
Analytic studies of a single boosted BH
  • Analytically studied case
  • Schwarzschild boosted with

Aichelburg-Sexl metric
  • Planar shock wave travelling along
  • Minkowskian everywhere else
  • No event horizon!

45
Analytic studies of a BH binary
  • Superpose two Aichelburg-Sexl metrics

Shock waves collide Penrose, Eardley Giddings
  • Future trapped surface!
  • Max. gravitational radiation
    Penrose
  • Perturb superposed Aichelburg-Sexl metrics

DEath Payne 90s
First correction term reduces GWs to
46
Analytic studies of a BH binary
  • Instant Collision approximation

Applied to superposed Aichelburg-Sexl
metric Smarr Adler Zeks
Energy spectrum
i) Flat at sufficiently low
ii) Radiation isotropic in the limit
iii) Functional relation
iv) Multipole structure
  • Numerical simulations Grand Challenge 90s

Limited accuracy, mild boosts
47
Numerical simulations
  • LEAN code Sperhake 07
  • Based on the Cactus computational toolkit
  • BSSN formulation
  • Puncture initial data Brandt Brügmann 1996
  • Elliptic solver TwoPunctures Ansorg 2005
  • Mesh refinement Carpet Schnetter 04
  • Numerically very challenging!
  • Length scales

Horizon Lorentz-contracted Pancake
  • Mergers extremely violent
  • Substantial amounts of unphysical junk
    radiation

48
Case example
  • Boost
  • initial separation
  • Total radiated energy
  • Mode energy
  • Junk radiation

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Modes
60
Modes
61
Modes
62
Modes
63
Modes
64
Modes
65
Energy spectrum
  • Junk radiation affects spectrum for small
    separations

66
Conclusions
  • Introduction to Numerical Relativity
  • NR has solved the binary problem
  • Key results on kicks, spin-flips, PN, data
    analysis
  • High energy collisions

Penrose limit
Numerical simulations very difficult (junk
radiation!)
Merger radiation for
  • Todo Improve accuracy, larger

67
Gravitational recoil
  • Anisotropic emission of GWs radiates momentum
  • recoil of remaining system
  • Leading order Overlap of Mass-quadrupole
  • with
    octopole/flux-quadrupole
  • Bonnor Rotenburg 61, Peres 62,
    Bekenstein 73
  • Merger of galaxies

Merger of BHs
Recoil
BH kicked out?
68
Gravitational recoil
  • Escape velocities

Globular clusters
dSph
dE
Giant galaxies
Merrit et al 04
  • Ejection or displacement of BHs has
    repercussions on
  • Structure formation in the universe
  • BH populations

IMBHs via ejection?
  • Growth history of Massive Black Holes
  • Structure of galaxies

69
Kicks of non-spinning black holes
  • Simulations PSU 07, Goddard 07
  • Parameter study Jena 07
  • Target Maximal Kick
  • Mass ratio
  • 150,000 CPU hours
  • Maximal kick
  • for
  • Convergence 2nd order
  • Spin

70
Super Kicks
  • Test Rochester-Prediction Jena 07
  • Two models

Lean Bam
  • Model I
  • Lean code
  • Moving puncture method version
  • Not quasi-circular
  • Resolutions
  • Model II Safety check with independent code
    BAM

71
Convergence
  • Discretization error
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