eiichiro komatsu & yuki watanabe university of texas at austin
DESCRIPTION
Reheating of the Universe after Inflation with f( f )R Gravity: Spontaneous Decay of Inflatons to Bosons, Fermions, and Gauge Bosons. Eiichiro Komatsu & Yuki Watanabe University of Texas at Austin Caltech High Energy Physics Seminar, March 28, 2007. - PowerPoint PPT PresentationTRANSCRIPT
Reheating of the Universe after Inflation with f()R Gravity:
Spontaneous Decay of Inflatons to Bosons, Fermions, and Gauge Bosons
Eiichiro Komatsu & Yuki WatanabeUniversity of Texas at Austin
Caltech High Energy Physics Seminar, March 28, 2007
Reference: Phys. Rev. D 75, 061301(R) (2007)
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Why Study Reheating?•The universe was left cold and empty after inflation.
•But, we need a hot Big Bang cosmology. •The universe must reheat after inflation.
Successful inflation must transfer energy in inflaton to radiation, and heat the universe to at least ~1 MeV for successful nucleosynthesis.
…however, little is known about this important epoch….
Outstanding Questions•Can one reheat universe successfully/naturally? •How much do we know about reheating? •What can we learn from observations (if possible at all)?•Can we use reheating to constrain inflationary models?•Can we use inflation to constrain reheating mechanism?
3/22
Standard Picture )(φV
φinflaton
Oscillation Phase: around the potential minimum at the end of inflati
on
Slow-roll Inflation: potential shape is arbitrary here, as long as it is flat.
inf2
2inf
24inf
4
4
~
~)(~
~
HMgT
HMgVg
T
Plrh
Pl
rhrad
⇒
φ
ρEnergetics:
What determines “energy-conversion efficiency factor”, g?
4/22
φ
φ
Perturbative ReheatingDolgov & Linde (1982); Abbott, Farhi & Wise (1982); Albrecht et al. (1982)
Thermal medium effect
Inflaton can decay if allowed kinematically with the widths given by
g g
⎟⎠
⎞⎜⎝
⎛ +++−= L42int 4
1λφφχψψφ χψ ggL
Pauli blocking
Bose condensateφ
φφ
φφ
φ
Inflaton decays and thermalizes through the tree-level interactions like:
5/22
Reheating Temperature from Energetics
Coupling constants determine the decay width, But, what determines coupling constants?
0)3( 2 =+++ φφφ σmH tot&&&
density.energy thedominate productsDecay 3
density.energy thedominatesInflaton 3
⇒<⇒>
totosc
totosc
HH
4*
22222 )(
3033)( rhrh
totPloscPlrhrad TTg
MHMt
πρ =
==
4/1
*4/12 100
)(
)10(
−
⎟⎠
⎞⎜⎝
⎛= rhtotPl
rhTgM
Tπ
2/3inf
−∝>> aHH oscφ
6/22
.10~then
, 10 and 10 If
~
7
6inf
10
inf2
−
−− ==
g
MHMT
HMgT
PlPlrh
Plrh
Fine-tuning Problem?
inf2
2inf
24inf
4
4
~
~)(~
~
HMgT
HMgVg
T
Plrh
Pl
rhrad
⇒
φ
ρ
To relax fine-tuning, one needs:(a)High reheat temperature
-> unwanted relics (e.g., gravitinos), (b)Very low-scale inflation (H~10-18 Mpl~10 GeV) -> worse fine-tuning, or
(c)Natural explanation for the smallness of g.
7/22
What are coupling constants? Problem: arbitrariness of the nature of inflaton fields
•Inflation works very well as a concept, but we do not understand the nature (including interaction properties) of inflaton.
•Arbitrariness of inflaton = Arbitrariness of couplings•Can we say anything generic about reheating? Universal reheating? Universal coupling?
e.g. Higgs-like scalar fields, Axion-like fields, Flat directions, RH sneutrino, Moduli fields, Distances between branes, and many more…
Gravitational coupling is universal
What happens to “gravitational decay channel”, when GR is modified?
-> however, too weak to cause reheating with GR.In the early universe, however, GR would be modified.
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Conventional Einstein gravity during inflation
( )L+++−= 222int χλφφχψψφ χψ ggL
Conventionally one had to introduce explicit couplings between inflaton and matter fields by hand.
Einstein-Hilbert term generates GR.Inflaton minimally couples to gravity.
mattLg−2PlM φφ νμ ∇∇
9/22
2)( PlMvf =
Modifying Einstein gravity during inflation
( )L+++−= 222int χλφφχψψφ χψ ggL
Instead of introducing explicit couplings by hand,
Non-minimal gravitational coupling: common in effective Lagrangian from e.g., extra dimensional theories.In order to ensure GR after inflation,
Matter (everything but gravity and inflaton) completely decouples from inflaton and minimally coupled to gravity as usual.
mattLg−φφ νμ ∇∇
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Field equations: GR
Linearized field equation:
Wave modes are gravitational waves. To identify the wave modes, we usually define
Harmonic (Lorenz) gauge:
2PlM φφ νμ ∇∇
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Field equations: f()R gravity
Linearized field equation during coherent oscillation
Wave modes are mixed up. To extract “true” gravitational degrees of freedom, we define
Harmonic (Lorenz) gauge:
φ
σ
v
φφ νμ ∇∇
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New decay channel through “scalar gravity waves”
Fermionic (spinor) matter field:
Bosonic (scalar) matter field:
Three-legged interaction
Yukawa interaction
g
σ
g
σ
g
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Spontaneous emergence of Yukawa interaction: analog of spontaneous symmetry breaking
.4
1
2
1
2
1 422 constL +⎟⎠
⎞⎜⎝
⎛ +−∂∂−= λφφμφφ μμ
⎟⎠
⎞⎜⎝
⎛ ++−∂∂−= 4322
4
1
2
1ληηληληη μ
μ vvL
)()( xvx ηφ +=
vλμ
φφ
λμ2
2
0)(
0 ,0
−=⇒=
∂
∂
><
vV
Expanding around the vev, one gets
-v
New term appeared.
14/22
)()( xvx σφ +=
( ) mLvvRvvgL +⎥⎦
⎤⎢⎣
⎡⎟⎠
⎞⎜⎝
⎛++−∇∇−++−= 432222
4
1
2
12
2
1λσσλσλσσξσσξξ μ
μ
( ) mLvRgL +⎥⎦
⎤⎢⎣
⎡−−∇∇−−=
2222
42
1
2
1φ
λφφξφ μ
μ
Wave mode mixing in the linear perturbations(appearance of scalar gravity waves)
σg σg
Spontaneous emergence of Yukawa interaction: analog of spontaneous symmetry breaking
Yukawa interactionsare induced.
Expanding around the vev, one gets
2)( ξφφ =fe.g.
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Magnitude of Yukawa coupling
For f()=ξg=ξ(v/Mpl)(m/Mpl) Natural to obtain g~10-7 for e.g., m~10-7 Mpl
The induced Yukawa coupling vanishes for massless fermions: conformal invariance of massless fermions.
Massless, minimally-coupled scalar fields are not conformally invariant. Therefore, the three-legged interaction does not vanish even for massless scalar fields:
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The Results So Far…
After inflation with f()R gravity, inflatons decay spontaneously into: Massive fermions, Massive scalar bosons, or Massless scalar bosons with non-conformal coupling.
The smallness of coupling can be explained naturally. Inflaton decay is “built-in” and the coupling constrants can be c
alculated explicitly from a single function, f(). Rates of decay to fermions and bosons are related.
This mechanism allows inflatons to decay into any fields that are not conformally coupled. Other possibilities?
Phys. Rev. D 75, 061301(R) (2007)
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Breaking of conformal invariance by anomaly
Example: decay to massless gauge bosons, F
Conformally coupled fields at the tree-level may not be conformally invariant when loops are included.
g
F
F
(c.f.) two-photon decay of the Higgs
€
α
€
α
18/22
Conformal anomaly: Lowest order decay channel to massless gauge fields
Inflaton -> 2 gauge fields
∞→→→→
xxI
xxI
as 0)(
0 as 3/1)(
g
F
F€
α
€
α
19/22
Decay Width Summary
Fermions
€
=f '(v)[ ]
2mψ
2mσ
32πM pl4
Scalar Bosons
€
=f '(v)[ ]
2mχ
2 +mσ
2
2
⎛
⎝ ⎜
⎞
⎠ ⎟
2
32πM pl4 mσ
Gauge Bosons
€
=α 2 f '(v)[ ]
2mσ
3
256π 3M pl4
× # of internal fermions etc( )
Probably the most dominant decay
channels
20/22
Constraint on f()R gravity models from reheating
4/1
*4/12 100
)(
)10(
−
⎟⎠
⎞⎜⎝
⎛= rhtotPl
rhTgM
Tπ
e.g.Constraints from chaotic inflation
999)Futamase(1&Komatsu
105||
)Maeda(1989&Futamase
10
4
3
λξ
ξ
×>
−> −
v
Trh
μμσ aa AAΓ+
2)( ξφφ =f
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Connection to Supergravity?
Similar effects have been pointed out by Endo, Takahashi and Yanagida (2006; 2007) in the context of supergravity Inflatons decay into any fields even if inflatons are not coupl
ed directly with these fields in the superpotentialA correspondence may be made as
f()R gravity <-> Kahler potentialConformal anomaly <-> Super-Weyl anomaly
Our model is simpler and does not require explicit use of supergravity -- hence more general. It may also give physical (rather than mathematical) insight i
nto their effects.
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Conclusions A natural mechanism for reheating after inflation with f()R gra
vity: Why natural? Inflaton quanta decay spontaneously into any matter fields (spin-0, ½,
1) without explicit interactions in the original Lagrangian Conformal invariance must be broken at the tree-level or by loops Reheating spontaneously occurs in any theories with f()R gravity
Predictability All the decay widths are related through a single function, f().
A constraint on f() from the reheat temperature can be found A possible limit on the reheat temperature can constrain the form of f(),
or vice versa. These constraints on f() are totally independent of the other constraints
from inflation and density fluctuations
Further Study… Preheating? F(,R) gravity?