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Perturbation and stability of higher dimensional black holes › media › cms_page_media › 436...
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Perturbation and stability of higher dimensional black holes
Akihiro Ishibashi GR 100 years in Lisbon
TECNICO, LISBON, 19 Dec. 2015
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Introduction Perturbation analysis: • GW emission from a particle plunging into or orbiting around a BH • Stability problem Stable final state of gravitational collapse Unstable New branch of solutions
• Information about the geometry: Quasi-Normal Modes • Insights into Uniqueness/non-uniqueness • Attempt to find new, approximate solutions
(by deforming an existing solution)
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Purpose of this talk A brief overview of linear perturbation theory of higher dimensional black holes
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Two major issues when formulating perturbation theory
• Fixing gauge ambiguity Imposing suitable gauge conditions
or Constructing manifestly gauge-invariant variables
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Two major issues when formulating perturbation theory
• Fixing gauge ambiguity Imposing suitable gauge conditions
or Constructing manifestly gauge-invariant variables • Reduction of perturbation equations to
a simple, tractable form (master equation) Classifying perturbations into mutually decoupled groups Separating variables
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4D master equations
Static asymptotically flat vacuum case Regge-Wheeler 57
Zerilli 70 charge case Moncrief
-- Stability Regge-Wheeler 57, Veshveshwara 70 …
asymptotically AdS/dS case Cardoso-Lemos
--- set of decoupled self-adjoint ODEs
Stationary Rotating vacuum (Kerr) case Teukolsky 72
--- Stability Press-Teukolsky 73 --- Whihting 89 …
asymptotically AdS/dS case Chambers-Moss 94
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• D>4 General Relativity No uniqueness like 4D GR Many unstable black (rotating) objects Uniqueness holds for “stable” black objects
Classification Problem in Higher Dimensions
Dynamical uniqueness theorem
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• Rotating BH case Not separable in general (e.g., Durkee-Godazgar-Reall) still a long way from having a complete perturbation theory Progress in some special cases Cohomogeneity-one (odd-dim. ) Myers-Perry BH Kunduri-Lucietti –Reall 07 (Tensor-modes ) Murata-Soda 08 (Tensor-Vector-Scalar modes) Single-spin (cohomogeneity-two) Myers-Perry Kodama-Konoplya-Zhidenko 09 Kundt spacetimes (e.g. Near-horizon geometry) Durkee-Reall 11 • Static BH case simpler and tractable:
-- can reduce to a set of decoupled s.a. ODEs Kodama-AI 03
Master equations for higher dimensional black holes
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Background geometry
: m – dim spacetime metric
: n – dim Einstein metric
-- corresponds to horizon-manifold
This metric can describe a fairly generic class of metrics
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FLRW universe
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FLRW universe
Static (Schwarzschild-type) black hole
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FLRW universe
Static (Schwarzschild-type) black hole
Black-brane
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FLRW universe
Static (Schwarzschild-type) black hole
Myers-Perry black hole ( w/ single rotation)
Black-brane
Kerr-brane
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Cosmological perturbation theory
: scale factor
: homogeneous isotropic time-slice
: FLRW background metric
Perturbations are decomposed into 3 types according to its tensorial behaviour on time-slice Tensor-type: transverse-traceless ( possible only when ) Gravitational Waves
Vectro-type: div-free vector couple to matter e.g. velocity perturbations Scalar-type: scalar couple to matter e.g. density perturbations
Gauge-invariant formulation Bardeen 80 Kodama-Sasaki 84
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Brane-world cosmology • AdS - (Black Hole)-Bulk spacetime
• Brane-world
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Brane-world cosmology • AdS - (Black Hole)-Bulk spacetime
• Brane-world
Bulk perturbations induce brane-world cosmological perturbations --- need to develop a formula for AdS-Black Hole perturbations --- convenient to decompose bulk perturbations into Tensor-, Vector-, Scalar-type wrt
Kodama – AI – Seto ‘00
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Black hole background geometry
charge
ADM-mass
Cosmological constant
Static solutions of Einstein-Maxwell + cosmological constant in
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Basic strategy to derive master equations (1) Mode-decompose as
Tensor-type new component in D > 4 case
Vector-type axial - mode in D = 4 case
Scalar-type polar - mode in D = 4 case
(2) Expand by tensor harmonics defined on
(3) Write the Einstein equations in terms of the expansion coefficients in 2-dim. spacetime spanned by
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Tensor-type perturbations
• : Transverse-Traceless harmonic tensor on
• is a gauge-invariant variable
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Tensor-type perturbations
• : Transverse-Traceless harmonic tensor on
• is a gauge-invariant variable
• Einstein’s equations reduce to Master equation
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Vector-type perturbations
• : Div.-free vector harmonics on :
• Gauge-invariant variable:
• Einstein’s equations reduce to
*
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Vector-type perturbations
• : Div.-free vector harmonics on :
• Gauge-invariant variable:
• Einstein’s equations reduce to
*
There exists such that
Einstein’s equation reduces to Master equation
-- corresponds to the Regge-Wheeler equation in 4D
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Scalar-type perturbations
• Construct gauge-invariant variables: on
• After Fourier transf. wrt ‘ ’ Einstein’s equations reduce to
• Expand by scalar harmonics on :
• Set of 1st –order ODEs for • A linear algebraic relation among them
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Scalar-type perturbations
• Construct gauge-invariant variables: on
• After Fourier transf. wrt ‘ ’ Einstein’s equations reduce to
--- such a system can be reduced to a single wave equation
• For a certain linear combination of
-- corresponds to the Zerilli equation in 4D
• Expand by scalar harmonics on :
• Set of 1st –order ODEs for • A linear algebraic relation among them
Einstein’s equations reduce to
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Stability analysis • Master equation takes the form:
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Stability analysis • Master equation takes the form:
If “ ” is a positive self-adjoint operator, the master equation does not admit “unstable” solutions
--- The black hole is stable
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Stability wrt Tensor-type
Stable
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Stability wrt Scalar-type
• Not obvious to see whether is positive or not …
The potential is NOT positive definite in D > 4
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Stability proof
• Define w. some function
where
Boundary terms vanish under the Dirichlet conditions
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Stability proof
• Define w. some function
where
Boundary terms vanish under the Dirichlet conditions
Task: Find that makes positive definite
Then, is uniquely extended to be a positive self-adjoint operator
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“OK” “Stable”
When the horizon manifold is maximally symmetric
WRT Tensor- and Vector-perturbations Stable over entire parameter range
WRT Scalar-perturbations ??? when
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Potential for Scalar-type pert. w. non-vanishing ,
For extremal and near-extremal case, the potential becomes negative in the immediate vicinity of the horizon
Numerical study for charged-AdS/dS case Konoplya-Zhidenko 07, 08, 09
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Some generalizations and open problems
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Static black holes in Lovelock theory
• Master equations in generic Lovelock theory Takahashi – Soda 10 in Gauss-Bonnet theory Dotti – Gleiser 05 • Asymptotically flat, small mass BHs are unstable wrt Tensor-type perturbations (in even-dim.) Scalar-type perturbations (in odd-dim.) • Instability is stronger in higher multipoles rather than low-multipoles
Higher curvature terms involved Equations of motion contain only up to 2nd-order derivatives
If , then for sufficiently large
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Rotating case: Cohomogeneity-2 Myers-Perry BHs
Numerical approach to stability analysis 5D bar-mode Shibata-Yoshino 10
--- include the ultra-spinning case
Axisymetric perturbation Dias-et. al. 09
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Cohomogeneity-2 MP case: Analytic formulation?
Tensor-type perturbations: A single master scalar variable on
satisfy the same equation for a massless Klein-Gordon field
How about vector-type and scalar-type perturbations?
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Cohomogeneity-2 MP case: Analytic formulation?
Tensor-type perturbations: A single master scalar variable on
satisfy the same equation for a massless Klein-Gordon field
How about vector-type and scalar-type perturbations?
KK-reduction along the Ricci flat space Equations for massive vector/ tensor fields on : 4-dim. Kerr metric
Kerr-brane: 4-dim. Kerr-metric + Ricci flat space
Pani, Gualtieri, Cardoso, AI 15
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Kunduri-Lucietti –Reall 07, Murata-Soda 08
c.f. Cohomogeneity-1 Myers-Perry BHs
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Canonical energy method for initial data
Symplectic current
Symplectic form
Canonical energy
Hollands-Wald 13
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Canonical energy method for initial data
Symplectic current
Symplectic form
Canonical energy
Hollands-Wald 13
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Canonical energy method for initial data
Symplectic current
Symplectic form
Canonical energy
Hollands-Wald 13
This method relates Dynamic and Thermodynamic stability criterion and proves Gubser-Mitra conjecture
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Role of symmetry in Stability problem
• Stability of extremal black holes Examine perturbations of the near-horizon geometry that respect the symmetry (axisymmetry) of the full BH solution
Conjectured by Durkee - Reall 11
Proven by use of Canonical energy method Hollands-AI 14
When axi-symmetric perturbations on the NHG violate -BF-bound on the NHG, then the original extremal BH is unstable
… supportd by numerical results. Dias et al
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Role of symmetry in Stability problem
• Stability of extremal black holes Examine perturbations of the near-horizon geometry that respect the symmetry (axisymmetry) of the full BH solution
Conjectured by Durkee - Reall 11
Proven by use of Canonical energy method Hollands-AI 14
When axi-symmetric perturbations on the NHG violate -BF-bound on the NHG, then the original extremal BH is unstable
… supportd by numerical results. Dias et al
Another application of Canonical energy method Superradiant instability of rotating AdS black holes Green-Hollands-AI-Wald 15 VIII BHworkshop
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Summary
• Static HDBHs: Complete formulation for perturbations
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Summary
• Static HDBHs: Complete formulation for perturbations • Rotating HDBHs: -- Still a long way from having a complete formulation -- Considerable progress recently made for some special
cases
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Summary • Static HDBHs: Complete formulation for perturbations • Rotating HDBHs: -- Still a long way from having a complete formulation -- Considerable progress recently made for some special
cases
• Interplay between Exact solutions + Perturbation analysis Numerical Analysis Mathematical Theorems
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1915 Einstein equations
Schwarzschild Solution 1915
1963
1957
1939
1965
1970
1982
Regge-Wheeler equation
Zerilli eqution
Singularity Theorems
Kerr solution
Oppenheimer-Snyder
1973
1975 BH Thermodynamcis laws Hawking radiation
Uniqueness Theorem
1983 Positive Energy Theorem
Interplay between Exact solutions + Perturbation Numerical Analysis Mathematical Theorems
Teukolsky equation
Exact Solutions + Perturbation analysis
Mathematica Theorems
Numerical Approach 1985 Accurate method to BH QNMs
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1986 Myers-Perry Solution
Gregory-Laflamme Instability
AdS-CFT correspondence
BTZ Solution
Brane-world scenario
1993
1997 1998
2001
2015
Emparan-Reall black ring
BSSN system in Numerical GR Choptuick’s critical collapse in Numerical GR
Exact solutions + Perturbation
Doubly spinning black ring Black saturn
Multiple- black rings
Black-lens Kunduri-Lucietti
HD BH Perturbation theory: This talk
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1986 Myers-Perry Solution
Gregory-Laflamme Instability
AdS-CFT correspondence
BTZ Solution
Brane-world scenario
1993
1997 1998
2001
2015
Emparan-Reall black ring
BSSN system in Numerical GR Choptuick’s critical collapse in Numerical GR
Numerical Analysis
High energy collisions of BHs Sperhake et al
Black-String final fate Lehner-Pretorius Bar-mode instability of MP BH Shibata-Yoshino Axisymmetric perturbation of MP BH – Dias et. al
Instability of AdS spacetimes – Bizon-Rostworowsky
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1986 Myers-Perry Solution
Gregory-Laflamme Instability
AdS-CFT correspondence
BTZ Solution
Brane-world scenario
1993
1997 1998
2001
2015
Emparan-Reall black ring
BSSN system in Numerical GR Choptuick’s critical collapse in Numerical GR
Mathematical Theorems
HD generalization of BH Topology Theorem HD generalization of BH rigidity (Symmetry) Theorem HD Uniqueness/Non-uniqueness Theorems
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1986 Myers-Perry Solution
Gregory-Laflamme Instability
AdS-CFT correspondence
BTZ Solution
Brane-world scenario
1993
1997 1998
2001
2015
Emparan-Reall black ring
Higher dimensional General Relativity
BSSN system in Numerical GR Choptuick’s critical collapse in Numerical GR
Interplay between Exact solutions + Perturbation Numerical Analysis Mathematical Theorems
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At GR Centenary • Perturbation theory has played a major role in understanding basic properties—e.g. stability—of exact solutions at hand. • Numerical Approach has become more important to reveal
interesting properties of complicated systems and/or to deal with more realistic models
• Mathematical theorems as guide lines
• Interplay between Numerical Approach Mathematical Theorems and Exact solution + Perturbation analysis will be getting more and more important .