black hole solutions in n>4 gauss-bonnet gravity
DESCRIPTION
4th International Seminar on High Energy Physics QUARKS'2006 Repino, St.Petersburg, Russia, May 19-25, 2006. Black hole solutions in N>4 Gauss-Bonnet Gravity. S.Alexeyev* 1 , N.Popov 2 , T.Strunina 3 1 S ternberg Astronomical Institute, Moscow, Russia - PowerPoint PPT PresentationTRANSCRIPT
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Black hole solutions in N>4 Gauss-Bonnet Gravity
S.Alexeyev*1, N.Popov2, T.Strunina3 1Sternberg Astronomical Institute, Moscow, Russia
2Computer Center of Russian Academy of Sciences, Moscow3Ural State University, Ekaterinburg, Russia
4th International Seminar on High Energy Physics QUARKS'2006Repino, St.Petersburg, Russia, May 19-25, 2006
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Main publications
S.Alexeyev and M.Pomazanov, Phys.Rev. D55, 2110 (1997)
S.Alexeyev, A.Barrau, G.Boudoul, M.Sazhin, O.Khovanskaya, Astronomy Letters 28, 489 (2002)
S.Alexeyev, A.Barrau, G.Boudoul, O.Khovanskaya, M.Sazhin, Class.Quant.Grav. 19, 4431 (2002)
A.Barrau, J.Grain, S.Alexeyev, Phys.Lett. B584, 114 (2004)
S.Alexeyev, N.Popov, A.Barrau, J.Grain, Journal of Physics: Conference Series 33, 343 (2006)
S.Alexeyev, N.Popov, T.Strunina, A.Barrau, J.Grain, in preparation
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Fundamental Planck scale shift
Large extra dimensions scenario (MD – D dimensional fundamental Planck mass, MPl – 4D Planck mass)
MD = [MPl2 / VD-4]
1/(D-2)
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Planck Energy shift
Planck energy in 4D representation
↓
1019 GeV
Fundamental Planck energy
↓
≈ 1 TeV
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Extended Schwarzschild solution in (4+n)D
Tangherlini, ‘1963, Myers & Perry, ‘1986
Metric:
ds2=-R(r)dt2+R(r)-1dr2+r2dΩn+22
Metric function: R(r) = 1 – [rs / r]n+1
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(4+n)D Low Energy Effective String Gravity
with higher order (second order in our consideration) curvature corrections
S=(16πG)-1∫dDx(-g)½[R + Λ + λ SGB + …]
Gauss-Bonnet term
SGB = Rμναβ Rμναβ – 4Rαβ Rαβ + R2
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Einstein-GB equations
R.Cai, ‘2003
Rµν - ½ gµνR - Λgµν
– α (½ gµνSGB – 2 RRµν + 4 RµγRγν
+ 4 RγδRγµ
δν – 2 RµγδλRν
γδν) = 0
SGB = Rμναβ Rμναβ – 4Rαβ Rαβ + R2
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(4+n)D Schwarzschild-Gauss-Bonnet black hole
solution(Boulware, Dieser, ‘1986, R.Cai, ‘2003)
Metric representation:
ds2 = - e2ν dt2 + e2α dr2 + r2 hij dxi dxj
Metric functions:
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Mass and Temperature
Mass
Temperature
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Hawking Temperature
M/MPl
M/MPl
Twith GB/Twithout GB
Twith GB/Twithout GB
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“Toy model”
(4+n)D Kerr-Gauss-Bonnet solution with one momentum (“degenerated solution”).
Necessity: to compare with the usual Kerr one in the complete range of dimensions: N=5,…,11
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“Degenerated” solution
here β(r,θ) is the function to be found, ρ2 = r2 + a2 cos2θ
N.Deruelle, Y.Morisawa, Class.Quant.Grav.22:933-938,2005, S.Alexeyev, N.Popov, A.Barrau, J.Grain, Journal of Physics: Conference Series 33, 343 (2006)
ds2 = - (du + dr)2 + dr2 + ρ2dθ2 + (r2 + a2) sin2θdφ2
+ 2 a sin2θ dr dφ + β(r,θ) (du – a sin2θ dφ)2
+ r2cos2θ (dx52 + sin2x5 (dx6
2 + sin2x6 (…dxN2)…)
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(UR) equation for β(r,θ)
For 6D case, for example
h1 = 24 α r3
h0 = r ρ2 (r2 + ρ2)g2 = 4 α (3r4 + 6 r2 a2 cos2θ – a4 cos4θ) / ρ2
g1 = (r2 + ρ2) (2r2 + ρ2)g0 = Λ r2 ρ4
[h1(r) β + h0(r,θ)] (dβ/dr)
+ [g2(r,θ) β2 + g1(r,θ) β + g0 (r,θ)] = 0
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Λ = 0
β(r,θ) μ /[rN-5 (r2 + a2 cos2θ)] + …
Λ ≠ 0
β(r,θ) C(N) Λ r4 / [r2 + a2 cos2θ] + …
Behavior at the infinity
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Behavior at the horizon
β(r,θ) = 1 + b1(θ) (r - rh) + b2(θ) (r – rh)2 + …
For 6D case
b1 = [4 α (3 rh4 + 6 rh
2 a2 cos2θ – a4 cos4θ) (rh2 + a2 cos2θ)-1
+ (2 rh2 + a2 cos2θ) (3 rh
2 + a2 cos2θ)
+ Λ rh2 (rh
2 + a2 cos2θ)2] / [24 α rh3 + rh (2 rh
2 + a2 cos2θ)]
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Usual form of metricds2 = - dt2 (1 – β2)
+ dr2 [(r4(1 – β2) + a2 (r2 + β2a2cos4θ) / Δ2]
+ ρ2dθ2 – 2aβ2sin2θ dtdφ + dφ2 sin2θ [r2 + a2 + a2β2 sin2θ]
+ r2 cos2θ (dx5 + …)
Δ = r2 + a2 - ρ2 β2
ρ2 = r2 + a2 cos2θ
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Mass & angular momentum
Mass M = µ (N-2) AN-2/16πG
where AN-1 = 2 πN/2/Γ(N/2)
Angular momentum Jyix
i = 2 M ai/N
the same as in pure Kerr case
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6D plot of β=β(r,a ∙ cosθ) in asymptotically flat case (Λ=0), λ=1
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6D plot of β=β(r,a ∙ cosθ) when Λ ≠ 0, λ=1
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While considering “degenerated solution” there are no any new types of particular points, so, there is no principal difference from pure Kerr case all the difference will occur only in temperature and its consequences
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Real angular momentum tensor
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Number of angular momentums
According to the existence of [Ns/2] Casimirs of SO(N) (Ns is the number of space dimensions) For N=4 (Ns=3) there is 1 moment
For N=5 (Ns=4) there are 2 moments
For N=6 (Ns=5) there are 2 moments
For N=7 (Ns=6) there are 3 moments
For N=8 (Ns=7) there are 3 moments
For N=9 (Ns=8) there are 4 moments
For N=10 (Ns=9) there are 4 moments
For N=11 (Ns=10) there are 5 moments
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5D Kerr metric (complete version)
ds2 = dt2 - dr2 - (r2+a2) sin2θ dφ1
- (r2+b2) cos2θ dφ2 – ρ2 dθ2
- 2 dr (a sin2θ dφ1 + b cos2θ dφ2)
- β (dt – dr – a sin2θ dφ1 - b cos2θ dφ2)Whereρ2 = r2 + a2 cos2θ + b2 sin2θ,β = β(r, θ) is unknown functiona, b - moments
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θθ component
A β’’ + B β’2 + C β’ + D β + E = 0
Where
A = r ρ2 (4 αβ – ρ2)
B = 4 α r ρ2
C = 2 [ 4 αβ (ρ2 - r2) – ρ2 (ρ2 + r2) ]
D = 2 r (2 r2 – 3 ρ2)
E = 2 r ρ4 Λ
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Solution manipulations
This equation could be divided into 2 parts
A(r,ρ)β’’+B(r,ρ)β’+C(r,ρ)β+D(r,ρ,Λ)=Z(r,ρ,β)
E(r,ρ)(ββ’)’+F(r,ρ)(ββ’) =Z(r,ρ,β)
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5D solution
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6D metric
ds2 = dt2 - dr2 – sin2ψ [(r2 + a2) sin2θ dφ12
+ (r2 + b2) cos2θ dφ22]
- (r2 + a2 cos2θ + b2 sin2θ) sin2ψ dθ2 - [r2 + (a2 sin2θ + b2 cos2θ) cos2ψ] dψ2 - 2 dr sin2ψ (a sin2θ dφ1 + b cos2θ dφ2) + 2 (b2 - a2) sinθ cosθ sinψ cosψ dθ dψ - β(r,θ,ψ) [dt – dr –sin2ψ (a sin2ψ dφ1 + b cos2θ dφ2)]2
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Conclusions
Taking into account 5D case one can see that in the general form of Kerr-Gauss-Bonnet solution there are no any new types of particular points, so, there is no principal difference from pure Kerr case all the difference will occur only in temperature and its consequences
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Thank you for your kind attention!And for your questions!