=1=Numerical simulations of coalescing binariessperhake/Talks/Slides/201408_QuyNhon.pdf ·...
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Numerical simulations of coalescing binaries
U. Sperhake
DAMTP, University of Cambridge
10th Rencontres du VietnamVery High Energy Phenomena in the Universe
Quy Nhon, 8th August 2014
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Overview
Introduction
Modelling of NSs, BHs in GR
Gravitational Wave Physics
Kicks and electromagnetic counterparts
Conclusions
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1. Introduction
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Neutron stars and stellar-mass BHs
NSsProgenitors stars
M? ∼ 8 . . . 40 (80?) M�
MNS & 1.4 . . . 2 M�
BHsProgenitor stars
M? & 20 M�
MBH ∼ 3 . . . 50 M�
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Supermassive BHs
Galaxies ubiquitously
harbor SMBHs
MBH ∼ 106 . . . 1010 M�
BH properties correlated
with bulge properties
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Evidence for astrophysical black holes
X-ray binaries
e. g. Cygnus X-1 (1964)
MS star + compact star
⇒ Stellar Mass BHs∼ 5 . . . 50 M�
Stellar dynamics
near galactic centers,
iron emission line profiles
⇒ Supermassive BHs
∼ 106 . . . 1010 M�
AGN engines
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Conjectured BHs
Intermediate mass BHs
∼ 102 . . . 105 M�
Primordial BHs
≤ MEarth
Mini BHs, LHC
∼ TeV
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Research areas of compact stars
Astrophysics
GW physics
Gauge-gravity duality
High-energy physics
Fundamental studies
Equation of state
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Luminosities
Lasers: . 1018 W
Tsar Bomba: ∼ 1026 W
GRB: ∼ 1045 W
Universe in electromagnetic radiation: ∼ 1049 W
Planck luminosity: 3.7× 1052 W
One BH binary can outshine the entire electromagnetic universe
Energy from 109 M� BH binary: EGW ∼ 1061 erg
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2. Modelling of NSs, BHs
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General Relativity: Curvature
Curvature generatesacceleration
“geodesic deviation”
No “force”!!
Description of geometry
Metric gαβ
Connection Γαβγ
Riemann Tensor Rαβγδ
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How to get the metric?
Train cemeteryUyuni, Bolivia
Solve for the metric gαβ
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How to get the metric?
Ricci-Tensor, Einstein Tensor, Matter Tensor
Rαβ ≡ Rµαµβ
Gαβ ≡ Rαβ − 12gαβRµ
µ “Trace reversed” Ricci
Tαβ “Matter”
Equations Gαβ = 8πTαβ , ∇µTµα = 0
2nd order PDEs for gαβ, matter Eqs.
Solutions: Easy! Take metric
⇒ Calculate Gαβ
⇒ Use that as matter tensor
Physically meaningful solutions: Difficult!
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Solving Einstein’s equations: Different methods
Analytic solutionsSymmetry: Schwarzschild, Kerr, FLRW, Oppenheimer-Snyder dust
Perturbation theoryAssume solution is close to known solution gαβ
Expand gαβ = gαβ + εh(1)αβ + ε2h(2)
αβ + . . . ⇒ linear system
Regge-Wheeler-Zerilli-Moncrief, Teukolsky, QNMs, EOB,...
Post-Newtonian TheoryAssume small velocities⇒ expansion in v
c
N th order expressions for GWs, momenta, orbits,...
Blanchet, Buonanno, Damour, Kidder, Will,...
Numerical RelativityBreakthroughs: Pretorius ’05, UT Brownsville ’05, NASA Goddard ’05
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A list of tasks
Matter: High-resolution shock capturing, Microphysics
Einstein equations: 1) Cast as evolution system
2) Choose specific formulation: BSSN, GHG
3) Discretize for computer
Choose coordinate conditions: Gauge
Fix technical aspects: 1) Mesh refinement / spectral domains
2) Singularity handling / excision
3) Parallelization
Construct realistic initial data
Start evolution...
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3. GW physics
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Gravitational wave detectors
Accelerated masses⇒ GWs
Weak interaction!
Laser interferometric detectors
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The gravitational wave spectrum
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Some targets of GW physics
Tests of GR
Hulse & Taylor 1993 Nobel Prize
Parameter determination
of BHs: M, ~S
Optical counter parts
Standard sirens (candles)
Test Kerr Nature of BHs
Neutron stars: EOS
BH formation scenarios
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Morphology of a BBH inspiral
Thanks to Caltech, CITA, Cornell
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Matched filtering
BH binaries have 7 parameters: 1 mass ratio, 2× 3 for spins
Sample parameter space, generate waveform for each point
NR + PN
Effective one body
GEO 600 noise
chirp signal
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Template construction
Stitch together PN and NR waveforms
EOB or phenomenological templates for ≥ 7-dim. par. space
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Template construction
Phenomenological waveform modelsModel phase, amplitude with simple functions→ Model parameters
Create map between physical and model parameters
Time or frequency domain
Ajith et al. 0704.3764, 0710.2335, 0712.0343, 0909.2867, Santamaria etal. 1005.3306, Sturani et al. 1012.5172, Hannam et al. 1308.3271
Effective-one-body (EOB) modelsParticle in effective metric, PN, ringdown modelBuonanno & Damour PRD ‘99, gr-qc/0001013
Resum PN, calibrate pseudo PN parameters using NRBuonanno et al. 0709.3839, Pan et al. 0912.3466, 1106.1021,1307.6232, Damour et al. 0712.202, 0803.3162, 1009.5998, 1406.6913
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The Ninja project
https://www.ninja-project.org/
Aylott et al, CQG 26 165008, CQG 26 114008
Ajith et al, CQG 29 124001
Use PN/NR hybrid waveforms in GW data analysis
Ninja2: 56 hybrid waveforms from 8 NR groups
Details on hybridization procedures
Overlap and mass bias study:Take one waveform as signal, fixing Mtot
Search with other waveform (same config.) varying t0, φ0, Mtot
Mass bias < 0.5 %
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The NRAR project
https://www.ninja-project.org/doku.php?id=nrar:home
Hinder, Buonanno et al. 1307.5307
Pool efforts from 9 NR groups
22 + 3 waveforms, including precessing runs
Standardize analysis, comparison with analytic models
Test EOB models with NR
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Tools of mass production
SpEC catalog: 171 waveforms: q ≤ 8, 90 precessing, ≤ 34 orbits
Mroué et al. 1304.6077
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Constraining the EOS of NSs with GWs
Step 1: Binary NS coalescence → char. frequency peaks
Takami et al. 1403.5672, Bauswein & Janka 1106.1616
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Constraining the EOS of NSs with GWs
Step 2: Relations f1 vs. M/R and f2 vs. M/R3
Takami et al. 1403.5672, Bauswein & Janka 1106.1616
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Constraining the EOS of NSs with GWs
Step 3: Combine with MTOV / RTOV curve and measured M
Takami et al. 1403.5672, Bauswein & Janka 1106.1616
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4. Kicks and electromagneticcounterparts
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SMBH formation
Most widely accepted scenario for galaxy formation:
hierarchical growth; “bottom-up”
Galaxies undergo frequent mergers⇒ BH merger
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Gravitational recoil
Anisotropic GW emission⇒ recoil of remnant BHBonnor & Rotenburg ’61, Peres ’62, Bekenstein ’73
Escape velocities: Globular clusters 30 km/s
dSph 20− 100 km/s
dE 100− 300 km/s
Giant galaxies ∼ 1000 km/s
Ejection / displacement of BH⇒
Growth history of SMBHs
BH populations, IMBHs
Displaced QSOs
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Kicks from non-spinning BHs
Max. kick: ∼ 180 km/s, harmless!
González et al., PRL 98, 091101 (2009)
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Spinning BHs: Superkicks
Kidder ’95, UTB-RIT ’07: maximum kick expected for
Kicks up to vmax ≈ 4 000 km/s
González et al. ’07, Campanelli et al. ’07
“Hang-up kicks” of up to 5 000 km/s Lousto & Zlochower ’12
Suppression via spin alignment and Resonance effects in inspiralSchnittman ’04, Bogdanovic et al. ’07, Kesden, US & Berti ’10, ’10a, ’12
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Neutron stars and γ-ray bursts
NS binaries can generate GRBs
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Double jets and spin flips
BH binary with plasma
Jets driven by L
Optical signature: double jets
Palenzuela, Lehner & Liebling ’10
Spin re-alignment
⇒ new + old jet
⇒ X-shaped radio sources
Campanelli et al. ’06
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5. Conclusions
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Conclusions
NR can reliably evolve compact binaries
PN results good for early inspiral of BHs, NSs
NR needed for merger
BHs, NSs important source of GWs
Some goals of GW physics:
EOS of NS matter, Standard Sirens, BH formation
Astrophysical studies: BH Kicks, Elm. signatures
Other physics: TeV Gravity, AdS/CFT, Fundamental physics
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Additional material forquestions
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3+1 Decomposition
GR: “Space and time exist as a unity: Spacetime”
NR: ADM 3+1 split Arnowitt, Deser & Misner ’62York ’79, Choquet-Bruhat & York ’80
gαβ =
(−α2 + βmβ
m βjβi γij
)3-Metric γijLapse αShift β i
lapse, shift⇒ Gauge
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ADM Equations
The Einstein equations Rαβ = 0 become6 Evolution equations
(∂t − Lβ)γij = −2αKij
(∂t − Lβ)Kij = −DiDjα + α[Rij − 2KimK mj + KijK ]
4 Constraints
R + K 2 − KijK ij = 0
−DjK ij + DiK = 0
preserved under evolution!
Evolution
1) Solve constraints
2) Evolve dataU. Sperhake (DAMTP, University of Cambridge)Numerical simulations of coalescing binaries 08/08/2014 41 / 53
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Formulations I: BSSN
One can easily change variables. E. g. wave equation
∂ttu − c∂xxu = 0 ⇔ ∂tF − c∂xG = 0
∂xF − ∂tG = 0
BSSN: rearrange degrees of freedom
χ = (det γ)−1/3 γij = χγij
K = γijK ij Aij = χ(Kij − 1
3γijK)
Γi = γmnΓimn = −∂mγ
im
Shibata & Nakamura ’95, Baumgarte & Shapiro ’98
BSSN strongly hyperbolic, but depends on details...
Sarbach et al.’02, Gundlach & Martín-García ’06
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Formulations I: BSSN
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Formulations II: Generalized harmonic (GHG)
Harmonic gauge: choose coordinates such that
∇µ∇µxα = 0
4-dim. version of Einstein equations
Rαβ = −12gµν∂µ∂νgαβ + . . .
Principal part of wave equation
Generalized harmonic gauge: Hα ≡ gαν∇µ∇µxν
⇒ Rαβ = −12gµν∂µ∂νgαβ + . . .− 1
2 (∂αHβ + ∂βHα)
Still principal part of wave equation !!! Manifestly hyperbolic
Friedrich ’85, Garfinkle ’02, Pretorius ’05
Constraint preservation; constraint satisfying BCs
Gundlach et al. ’05, Lindblom et al. ’06
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Discretization of the time evolution
Finite differencing (FD)
Pretorius, RIT, Goddard, Georgia Tech, LEAN, BAM, UIUC,...
Spectral Caltech-Cornell-CITA
Parallelization with MPI, ∼ 128 cores, ∼ 256 Gb RAM
Example: advection equation ∂t f = ∂x f , FD
Array f nk for fixed n
f n+1k = f n
k + ∆tf nk+1−f n
k−12∆x
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Initial data
Two problems: Constraints, realistic data
Rearrange degrees of freedom
York-Lichnerowicz split: γij = ψ4γij
Kij = Aij + 13γijK
York & Lichnerozwicz, O’Murchadha & York,
Wilson & Mathews, York
Make simplifying assumptions
Conformal flatness: γij = δij , and K = 0
Find good elliptic solvers, e. g. Ansorg et al. ’04
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Mesh refinement
3 Length scales : BH ∼ 1 M
Wavelength ∼ 10...100 M
Wave zone ∼ 100...1000 M
Critical phenomena
Choptuik ’93
First used for BBHs
Brügmann ’96
Available Packages:
Paramesh MacNeice et al. ’00
Carpet Schnetter et al. ’03
SAMRAI MacNeice et al. ’00
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The gauge freedom
Remember: Einstein equations say nothing about α, β i
Any choice of lapse and shift gives a solution
This represents the coordinate freedom of GR
Physics do not depend on α, β i
So why bother?
The performance of the numerics DO depend strongly on thegauge!
How do we get good gauge?
Singularity avoidance, avoid coordinate stretching, well posedness
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What goes wrong with bad gauge?
U. Sperhake (DAMTP, University of Cambridge)Numerical simulations of coalescing binaries 08/08/2014 49 / 53
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What goes wrong with bad gauge?
U. Sperhake (DAMTP, University of Cambridge)Numerical simulations of coalescing binaries 08/08/2014 50 / 53
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What goes wrong with bad gauge?
U. Sperhake (DAMTP, University of Cambridge)Numerical simulations of coalescing binaries 08/08/2014 51 / 53
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What goes wrong with bad gauge?
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A brief history of BH simulations
Pioneers: Hahn & Lindquist ’60s, Eppley, Smarr et al. ’70s
Grand Challenge: First 3D Code Anninos et al. ’90s
Further attempts: Bona & Massó, Pitt-PSU-Texas
AEI-Potsdam, Alcubierre et al.
PSU: first orbit Brügmann et al. ’04
Codes unstable!
Breakthrough: Pretorius ’05 GHG
UTB, Goddard’05 Moving Punctures
Currently about 10 codes world wide
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