new bubbles in cosmologyias.ust.hk/workshop/cosmology/2014/doc/lee.pdf · 1. motivation &...
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New Bubbles in Cosmology
Bum-Hoon Lee Center for Quantum SpaceTime/Department of Physics
Sogang University, Seoul, Korea
HKUST, Hongkong May 19, 2014
Contents 1. Motivation & Basics, Basics – bubbles in the flat spacetime
2. Bubble nucleation in the Einstein gravity 3. More Bubbles and Tunneling 3.1.False vacuum bubble nucleation 3,2 vacuum bubbles with finite geometry 3.3 Tunneling between the degenerate vacua 3.4 Oscillaing solutions 3.5.Fubini Instanton in Gravity 4. Possible Cosmological Implication 5. Summary and discussions
1. Motivation & Basics
Bubbles (*) For Phase Tran. in the early universe with or w/o cosmol. constants, Can we obtain the mechanism for the nucleation of a false vac bubble? Can a false vacuum bubble expand within the true vacuum background?
How can we be in the vacuum with positive cosmol const ? - KKLT(Kachru,Kallosh,Linde,Trivedi, PRD 2003)) : “lifting” the potential - an alternative way? : Revisit the gravity effect in cosmol. phase trans.
We will revisit and analyse vacuum bubbles in various setup.
Observation : Universe is expanding with acceleration - needs positive cosmological constant
The string theory landscape provides a vast number of metastable vacua.
AdS dS KKLT
(*) Other possible roles of the Euclidean Bubbles and Walls? Ex) quantum cosmology? Domain Wall Universe?
Basics : Bubble formation
)](1[/ / Ο+=Γ −BAeV
Vacuum-to-vacuum phase transition rate
B : Euclidean Action (semiclassical approx.) S. Coleman, PRD 15, 2929 (1977) S. Coleman and F. De Luccia, PRD21, 3305 (1980) S. Parke, PLB121, 313 (1983) A : determinant factor from the quantum correction C. G. Callan and S. Coleman, PRD 16, 1762 (1977)
- Nonperturbative Quantum Tunneling
q σ
V “True” vacuum
“False” vacuum
(1) Tunneling in Quantum Mechanics - particle in one dim. with unit mass -
Lagrangian
Quantum Tunneling:(Euclidean time -∞<τ <0 or 0<τ<∞) The particle (at “false vacuum” q0) penetrates the potential barrier and materializes at the escape point, σ , with zero kinetic energy,
where = Classical Euclidean action (difference) Eq. of motion : boundary conditions
)](1[/ / Ο+=Γ −BAeVTunneling probability
Time evolution after tunneling : (back to Minkowski time, t > 0) Classical Propagation after tunneling (at τ = 0=t)
0|,)( )(0lim == =−∞→
σττ η
τddqqq o
-V
q
q
σ
V
σ
“True” vacuum
“False” vacuum
→ The bounce solution is a particle moving in the potential –V in time τ is unstable (exists a mode w/ negative eigenvalue)
it=τ
q0
q0
+
-∞
∞
at τ=0
at τ=-∞ (and +∞)
(2) Tunneling in multidimension
Lagrangian
)(21 qVqqL j
iji −=
••
∑The leading approx. to the tunneling rate is obtained from the path and endpoints that minimize the tunneling exponent B. Boundary conditions for the bounce
0)()( == ioi VqV σ
iσ
∫ ∫∞
∞−===
2
1
2/1)2(2S
S EE SLdVdsB τ
→
→
∂
∂=
q
Vd
qd2
2
τ0=∫ b
ELdτδ Vd
qdd
qdLE +•=
→→
ττ21
0|,)( )(0lim == =−∞→
iddqqq i
oii σττ τ
η
Time evolution after the tunneling is classical with the ordinary Minkowski time.
(3) Tunneling in field theory (in flat spacetime – no gravity )
Theory with single scalar field where
Φ−Φ∇Φ∇−−= ∫ )(
214 UxdS α
αη
,det µνηη = ),,,( +++−
True vacuum False vacuum Equation for the bounce
with boundary conditions
Tunneling rate :
(Finite size bubble)
0=∫ bELdτδ
)'(2
2
2
Φ=Φ
∇+
∂∂
Uτ
Fx Φ=Φ→
±∞→
),(lim ττ
F
x
x Φ=Φ→
∞→→
),(lim||
τ0),0( =∂Φ∂ →
xτ
Φ+Φ∇+
∂Φ∂
==→
∫ )()(21
21 2
23 UxddSB E τ
τ
V
)](1[/ / Ο+=Γ −BAeV
O(4)-symmetry : Rotationally invariant Euclidean metric
)]sin(sin[ 22222222 φθθχχηη ddddds +++= )( 222 r+=τη
Φ=Φ+Φ
d
dU'
3''η
0|,)( 0lim =Φ
Φ=Φ =∞→
ηη η
ηdd
F
Tunneling probability factor
Φ+
∂Φ∂
== ∫∞
)(212
2
0
32 UdSB E ηηηπ
The Euclidean field equations & boundary conditions
“Particle” Analogy : (at position Ф at time η)
The motion of a particle in the potential –U with the damping force proportional to 1/ η.
ηηητ d
d
d
d 32
22
2
2
+=∇+∂∂
( )
at τ=0 at τ=+∞
Thin-wall approximation
B is the difference
in wall outB B B B= + +
FE
bE SSB −=
)(2
)(8
)( 222 bb
bU −Φ−−Φ=Φελ
(ε: small parameter)
True vacuum
False vacuum
R
Large 4dim. spherical bubble with radius R and thin wall
Bubble solution
R In this approximation
the radius of a true vacuum bubble
ΦΦ−Φ= ∫Φ
ΦdUUS F
TTo )]()([2
εηπ 42
21
−=inB
,2 32owall SB ηπ=
εη /3 oS=
3
42
227
επ o
EoSSB ==
true vacuum
False vacuum
- ≡R
on the wall
Inside the wall
the nucleation rate of a true vacuum bubble
where
0)()( =Φ−Φ= FEFEout SSB
Outside the wall
False vacuum
FE
bE SSB −=
in wall outB B B B= + +
Evolution of the bubble
The false vacuum makes a quantum tunneling into a true vacuum bubble at time τ=t=0, such that
Afterwards, it evolves according to the classical equation of motion in Lorentzian spacetime.
The solution (by analytic continuation)
.0),0(
),0(),0(
==Φ∂∂
=Φ==Φ→
→→
xtt
xxt τ
)('22
2
Φ=Φ∇+∂Φ∂
− Ut
))|(|(),( 2/122 txxt −=Φ=Φ→→
η
(Note: Φ is a function of η ) )( 222 r+=τη
True vacuum
False vacuum
τ=0
R
That is, the initial condition is given by the τ=t=0 slice at rest.
τ
t
r
2. Bubble nucleation in the Einstein gravity
Action
2 2 2 2 2 2 2 2( )[ sin ( sin )]ds d d d dη ρ η χ χ θ θ φ= + + +
boundarySURxdgS +
Φ−Φ∇Φ∇−= ∫ )(
21
24
αα
κ
S. Coleman and F. De Luccia, PRD21, 3305 (1980)
Φ=Φ+Φ
ddU''3''
ρρ
0|,)( 0(max)
lim =Φ
Φ=Φ =→
ηηη η
ηdd
F
)'21(
31' 2
22 U−Φ+=
κρρ
O(4)-symmetric Euclidean metric Ansatz
The Euclidean field equations (scalar eq. & Einstein eq.)
boundary conditions for bubbles
the nucleation rate
2)2/(1 Λ+= −
−−
η
ηρ
2/1)3/( −=Λ κε
22 ])2/(1[ Λ+= −
η
oBB
2)2/(1 Λ−= −
−−
η
ηρ
22 ])2/(1[ Λ−= −
η
oBBthe nucleation rate
(i) From de Sitter to flat spacetime
the radius of the bubble
where
Minkowski dS
(ii) From flat to Anti-de Sitter spacetime
the radius of the bubble
Minkowski AdS
(iii) the case of arbitrary vacuum energy
+
+
−
+
+−
+
=−−−
−−−
2/14
2
2
1
2
1
2
4
2
2/14
2
2
1
2
1
22211
2
2221
212
λη
λη
λλ
λη
λη
λη
λη
o
p
B
B
+
+
=−−
−
4
2
2
1
2
2
2221
λη
λη
ηρ p )](/3[21 TF UU −= κλ 2
2 [3 / ( )]F TU Uλ κ= +
• Evolution of the bubble
→ via analytic continuation back to Lorentzian time
Ex) de Sitter → de Sitter : A. Brown & E. Weinberg, PRD 2007
the radius
the nucleation rate
S. Parke, PLB121, 313 (1983)
AdS→AdS
flat→AdS dS→AdS
dS→flat
dS→dS
Note : Analytic continuation in the presence of gravity is nontrivial.
Homogeneous tunneling A channel of the inhomogeneous tunneling
Ordinary bounce (vacuum bubble) solutions
before after
A channel of the homogeneous tunneling
Hawking-Moss instanton
before after
- The Einstein theory of gravity with a nonminimally coupled scalar field
Einstein equations
4 21 1[ ( )]2 2 2RS gd x R Uα
α ξκ
= − ∇ Φ∇ Φ− Φ − Φ∫
12
R g R Tµν µν µνκ− =
2 22
1 1[ ( ) ( )]1 2
T g U gα αµν µ ν µν α µν α µ νξ
ξ κ= ∇ Φ∇ Φ− ∇ Φ∇ Φ+ + ∇ ∇ Φ −∇ ∇ Φ
− Φ
boundaryS+
3.1 False vacuum bubble nucleation
Action
curvature scalar
κξξκ µ
µµ
µ
2
2
1]3)(4[
Φ−Φ∇∇−Φ∇Φ∇+Φ
=U
R
Potential
2 2( ) ( 2 ) ( 2 )8 2 oU b b U
bλ ε
Φ = Φ Φ− − Φ − +
3. More Bubbles and Tunneling
False vacuum bubble
True vacuum bubble
boundary conditions
2 2 2 2 2 2 2 2( )[ sin ( sin )]ds d d d dη ρ η χ χ θ θ φ= + + +
3 ''' ' EdURd
ρ ξρ
Φ + Φ − Φ =Φ
22 2
2
1' 1 ( ' )3(1 ) 2
Uκρρξ κ
= + Φ −− Φ
0|,)( 0(max)
lim =Φ
Φ=Φ =→
ηηη η
ηdd
T
Rotationally invariant Euclidean metric : O(4)-symmetry
The Euclidean field equations
Our main idea
3 ' 'ER ρξρ
Φ > Φ
(during the phase transition)
False-to-true
(True vac. Bubble)
True-to-false (*)
(False vac. Bubble)
De Sitter – de Sitter O O (*)
Flat – de Sitter O O
Anti de Sitter – de Sitter O O
Anti de Sitter – flat O O
Anti de Sitter – Anti de Sitter O O
(*) exists in
(1)non-minimally coupled gravity
or in
(2)Brans-Dicke type theory
(W.Lee, BHL, C.H.Lee,C.Park, PRD(2006))
(*)Lee, Weinberg, PRD
Dynamics of False Vacuum Bubble :
Can exist an expanding false vac bubble inside the true vacuum
BHL, C.H.Lee, W.Lee, S. Nam, C.Park, PRD(2008) (for nonminimal coupling)
True & False Vacuum Bubbles
BHL, W.Lee, D.-H. Yeom, JCAP(2011) (for Brans-Dicke)
(H.Kim,BHL,W.Lee, Y.J. Lee, D.-H.Yoem, PRD(2011))
X
AdS→AdS
flat→AdS
dS→AdS dS→flat
dS→dS
True Vac Bubble
False Vac Bubble
dS-dS dS-AdS
dS-flat flat-AdS and AdS-AdS
η η
ρ
Φ
3.2 vacuum bubbles with finite geometry BHL, C.H. Lee, W.Lee & C.Oh,
Boundary condition (consistent with Z2-sym.)
- in de Sitter space.
The numerical solution by Hackworth and Weinberg.
The analytic computation and interpretation :
(BHL & W. Lee, CQG (2009))
3.3 Tunneling between the degenerate vacua ∃ Z2-symm. with finite geometry bubble
Potential
Equations of motions
O(4)-symmetric Euclidean metric
)( 222 r+=τη2 2 2 2 2 2 2 2( )[ sin ( sin )]ds d d d dη ρ η χ χ θ θ φ= + + +
dS - dS
flat -flat
AdS-AdS
B.-H. L, C. H. Lee, W. Lee & C. Oh, PRD82 (2010)
3.3 Oscillaing solutions : a) between flat-flat degenerate vacua ( )
27
B.-H. Lee, C. H. Lee, W. Lee & C. Oh, arXiv:1106.5865
This type of solutions is possible only if gravity is taken into account.
energy density
30
3.3 Oscillaing solutions - b) between dS-dS degenerate vacua
31
3.3 Oscillaing solutions – c) between AdS-AdS degenerate vacua
33
The phase space of solutions
36
The y-axis represents no gravity. the notation (n_min, n_max), where n_min means the minimum number of oscillations and n_max the maximum number of oscillation
37
the schematic diagram of the phase space of all solutions including another type solution and the number of oscillating solutions with different κs. The left figure has κ = 0 line indicating no gravity effect. In the middle area including the flat case, n_min and n_max are increased as κ and κUo are decreased. The tendencies are indicated as the arrows. In the left lower region, there exist another type solution. The right figure shows n_min and n_max are changed in terms of κUo and κ. As we can see from the figure, n_max and n_min are increased as κUo is decreased.
Review : In the Absence of Gravity
• Fubini, Nuovo Cimento 34A (1976) • Lipatov – JETP45 (1977)
action
Equation of motion
Boundary conditions
solution
3.4 Fubini Instanton in Gravity
In the Presence of Gravity
Action
O(4) symmetric metric
Equantions of motion
Boundary Conditions
B-HL, W. Lee, C.Oh, D. Yeom, D. Rho JHEP 1306 (2013) 003; in preparation
After the nucleation, the domain wall (that may be interpreted as our braneworld universe) evolves in the radial direction of the bulk spacetime.
λ = 3A : the effective cosmological constant. mass term ~ the radiation in the universe charge term ~ the stiff matter with a negative energy density.
Cosmological solutions
the expanding domain wall (universe) solution (a > r∗,+). approaching the de Sitter inflation with λ, since the contributions of the mass and charge terms are diluted. contracting solution (a < r∗,+) : the initially collapsing universe. The domain wall does not run into the singularity & experiences a bounce since there is the barrier in V (a) because of the charge q.
The equation becomes
4.1 5Dim. Z2 symmetric Black hole with a domain wall solution.
4. Possible Cosmological Implication
4.2 Application to the No-boundary
to avoid the singularity problem of a Universe
the no-boundary proposal by Hartle and Hawking cf) Vilenkin’s tunneling boundary condition
before
nothing
after
Something, homogeneous
the ground state wave function of the universe is given by the Euclidean path integral satisfying the WD equation
Consider the Euclidean action
the mini-superspace approximation => the scale factor as the only dof.
The equations of motion
the regular initial conditions at
We want to analytically continue the solution to the Lorentzian manifold using Then at the tunneling point we have to impose the followings
9
12
13
4.3 General vacuum decay problem
4.4 False Cosmic String and its Decay
Acton
Vortex Solution
B-HL, W. Lee, R. MacKenzie, M.Paranjape U. Yajnik, D-h Yeom. PRD88 (2013) 085031 arXiv:1308.3501 PRD88 (2013) 105008 arXiv:1310.3005
Decay of the False String (thin wall approximation)
Tunnelling Solution
5. Summary and Discussions
We reviewed the formulation of the bubble. False vacua exist e.g., in non-minimally coupled theory.
Vacuum bubbles with finite geometry, with the radius & nucleation rate New Type of the solutions : Ex) bubble with compact geometry, degenerate vacua in dS, flat, & AdS. Oscillating solutions; can make the thick domain wall.
Similar analysis for the Fubini instanton
Physical role and interpretation of many solutions are still not clear.
The application to the braneworld cosmology has been discussed for the model of magnetically charged BH pairs separated by a domain wall in the 4 or 5-dim. spacetime with a cosmological constant. Can there be alternative model for the accelerating expanding universe?