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The Origin of Matter
Ewan Stewart
KAIST
Physics Colloquium4 May 2009
Dept. of Physics, KAIST
The Origin of Matter
The Standard Model
Beyond the Standard Model
Big Bang cosmology
A theory for the origin of matter
The Origin of Matter
The Standard ModelOrdinary matterQuarksNeutrinosHiggs boson
Beyond the Standard ModelNeutrino massesSupersymmetryAxionsGravitinos and moduliParticle spectrum
Big Bang cosmologyThe hot Big BangPrimordial inflationMatter/antimatter asymmetryDark matterGravitinos and moduli
A theory for the origin of matterA Minimal Supersymmetric Cosmological ModelThermal inflationBaryogenesisDark matterHistory of the observable universe
Ordinary matter
atom = electrons
photons
+ nucleus
nucleus = protons + neutrons
Ordinary matter
atom = electronsphotons
+ nucleus
nucleus = protons + neutrons
Ordinary matter
atom = electronsphotons
+ nucleus
nucleus = protons + neutrons
Particle spectrum
electron
neutronproton
photon graviton
Quarks
proton = up quark
gluons
+ up quark
gluons
+ down quark
neutron = up quark
gluons
+ down quark
gluons
+ down quark
Quarks
proton = up quarkgluons
+ up quarkgluons
+ down quark
neutron = up quarkgluons
+ down quarkgluons
+ down quark
Particle spectrum
electron
neutronproton
photon graviton
Particle spectrum
Quarks Strong
electron
neutronproton
photon graviton
Particle spectrum
Quarks Strong
electron
downup
photon
gluon
graviton
Particle spectrum
Quarks Strong
electron
top
bottomcharm
strange
downup
photon
gluon
graviton
Neutrinos
In the Sunproton + proton→ deuterium + antielectron + neutrino
Trillions of neutrinos pass through us every second!
neutrino interactions
electromagneticstrong nuclearweak nucleargravitational
The weak nuclear force is mediated by the W and Z bosons
upquark
downquark
Wantielectron
neutrino
The W and Z bosons are massive and hence do not give rise to a long range force.The electromagnetic and weak nuclear forces are unified into the electroweak force.
Neutrinos
In the Sunproton + proton→ deuterium + antielectron + neutrino
Trillions of neutrinos pass through us every second!
neutrino interactions
electromagneticstrong nuclearweak nucleargravitational
The weak nuclear force is mediated by the W and Z bosons
upquark
downquark
Wantielectron
neutrino
The W and Z bosons are massive and hence do not give rise to a long range force.The electromagnetic and weak nuclear forces are unified into the electroweak force.
Neutrinos
In the Sunproton + proton→ deuterium + antielectron + neutrino
Trillions of neutrinos pass through us every second!
neutrino interactions
electromagneticstrong nuclearweak nucleargravitational
The weak nuclear force is mediated by the W and Z bosons
upquark
downquark
Wantielectron
neutrino
The W and Z bosons are massive and hence do not give rise to a long range force.The electromagnetic and weak nuclear forces are unified into the electroweak force.
Neutrinos
In the Sunproton + proton→ deuterium + antielectron + neutrino
Trillions of neutrinos pass through us every second!
neutrino interactions
electromagneticstrong nuclearweak nucleargravitational
The weak nuclear force is mediated by the W and Z bosons
upquark
downquark
Wantielectron
neutrino
The W and Z bosons are massive and hence do not give rise to a long range force.The electromagnetic and weak nuclear forces are unified into the electroweak force.
Neutrinos
In the Sunproton + proton→ deuterium + antielectron + neutrino
Trillions of neutrinos pass through us every second!
neutrino interactions
electromagneticstrong nuclearweak nucleargravitational
The weak nuclear force is mediated by the W and Z bosons
upquark
downquark
Wantielectron
neutrino
The W and Z bosons are massive and hence do not give rise to a long range force.The electromagnetic and weak nuclear forces are unified into the electroweak force.
Neutrinos
In the Sunproton + proton→ deuterium + antielectron + neutrino
Trillions of neutrinos pass through us every second!
neutrino interactions
electromagneticstrong nuclearweak nucleargravitational
The weak nuclear force is mediated by the W and Z bosons
upquark
downquark
Wantielectron
neutrino
The W and Z bosons are massive and hence do not give rise to a long range force.
The electromagnetic and weak nuclear forces are unified into the electroweak force.
Neutrinos
In the Sunproton + proton→ deuterium + antielectron + neutrino
Trillions of neutrinos pass through us every second!
neutrino interactions
electromagneticstrong nuclearweak nucleargravitational
The weak nuclear force is mediated by the W and Z bosons
upquark
downquark
Wantielectron
neutrino
The W and Z bosons are massive and hence do not give rise to a long range force.The electromagnetic and weak nuclear forces are unified into the electroweak force.
Particle spectrum
Quarks Strong
electron
top
bottomcharm
strange
downup
photon
gluon
graviton
Particle spectrum
Quarks Strong
electron
neutrinos
top
bottomcharm
strange
downup
photon
gluon
graviton
Particle spectrum
Leptons Quarks Electroweak Strong
electron
neutrinos
top
bottomcharm
strange
downup
photon
gluon
graviton
Particle spectrum
Leptons Quarks Electroweak Strong
electron
neutrinos
top
bottomcharm
strange
downup
photon
Z W
gluon
graviton
Particle spectrum
Leptons Quarks Electroweak Strong
tau
muon
electron
neutrinos
top
bottomcharm
strange
downup
photon
Z W
gluon
graviton
Higgs boson
The Higgs boson couples to the quarks and leptons in the Standard Model
λuQHu + λdQHd + λeLHe
→ muuu + mddd + meee
where
Q =
(ud
), L =
(νe
)
, H →(
0h
)When the Higgs boson acquires a non-zero value, it gives mass to the quarks andelectron
mu = λuh , md = λdh∗ , me = λeh∗
It similarly gives masses to the W and Z bosons.
Higgs boson
The Higgs boson couples to the quarks and leptons in the Standard Model
λuQHu + λdQHd + λeLHe
→ muuu + mddd + meee
where
Q =
(ud
), L =
(νe
), H →
(0h
)When the Higgs boson acquires a non-zero value,
it gives mass to the quarks andelectron
mu = λuh , md = λdh∗ , me = λeh∗
It similarly gives masses to the W and Z bosons.
Higgs boson
The Higgs boson couples to the quarks and leptons in the Standard Model
λuQHu + λdQHd + λeLHe → muuu + mddd + meee
where
Q =
(ud
), L =
(νe
), H →
(0h
)When the Higgs boson acquires a non-zero value, it gives mass to the quarks andelectron
mu = λuh , md = λdh∗ , me = λeh∗
It similarly gives masses to the W and Z bosons.
Higgs boson
The Higgs boson couples to the quarks and leptons in the Standard Model
λuQHu + λdQHd + λeLHe → muuu + mddd + meee
where
Q =
(ud
), L =
(νe
), H →
(0h
)When the Higgs boson acquires a non-zero value, it gives mass to the quarks andelectron
mu = λuh , md = λdh∗ , me = λeh∗
It similarly gives masses to the W and Z bosons.
Particle spectrum
Leptons Quarks Electroweak Strong
tau
muon
electron
neutrinos
top
bottomcharm
strange
downup
photon
Z W
gluon
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
tau
muon
electron
neutrinos
top
bottomcharm
strange
downup
Higgs
photon
Z W
gluon
graviton
The Origin of Matter
The Standard ModelOrdinary matterQuarksNeutrinosHiggs boson
Beyond the Standard ModelNeutrino massesSupersymmetryAxionsGravitinos and moduliParticle spectrum
Big Bang cosmologyThe hot Big BangPrimordial inflationMatter/antimatter asymmetryDark matterGravitinos and moduli
A theory for the origin of matterA Minimal Supersymmetric Cosmological ModelThermal inflationBaryogenesisDark matterHistory of the observable universe
Neutrino masses
Neutrinos have no mass in the Standard Model. However, in reality one expects higherorder couplings including
1
2λν (LH)2
→1
2mνν
2
where
L =
(νe
)
, H →(
0h
)When the Higgs boson acquires a non-zero value, it gives small masses to the neutrinos
mν = λνh2
in agreement with observations.
Neutrino masses
Neutrinos have no mass in the Standard Model. However, in reality one expects higherorder couplings including
1
2λν (LH)2
→1
2mνν
2
where
L =
(νe
), H →
(0h
)When the Higgs boson acquires a non-zero value,
it gives small masses to the neutrinos
mν = λνh2
in agreement with observations.
Neutrino masses
Neutrinos have no mass in the Standard Model. However, in reality one expects higherorder couplings including
1
2λν (LH)2 →
1
2mνν
2
where
L =
(νe
), H →
(0h
)When the Higgs boson acquires a non-zero value, it gives small masses to the neutrinos
mν = λνh2
in agreement with observations.
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
tau
muon
electron
neutrinos
top
bottomcharm
strange
downup
Higgs
photon
Z W
gluon
graviton
Supersymmetry
Supersymmetry is a symmetry between bosons and fermions
bosonsusy←→ fermion
It extends Poincare symmetry {Q, Q
}∼ P
In a supersymmetric field theory, fields are replaced by superfields, which contain bothbosons and fermions
field→ superfield =
(boson
fermion
)
Supersymmetry
Supersymmetry is a symmetry between bosons and fermions
bosonsusy←→ fermion
It extends Poincare symmetry {Q, Q
}∼ P
In a supersymmetric field theory, fields are replaced by superfields, which contain bothbosons and fermions
field→ superfield =
(boson
fermion
)
Supersymmetry
Supersymmetry is a symmetry between bosons and fermions
bosonsusy←→ fermion
It extends Poincare symmetry {Q, Q
}∼ P
In a supersymmetric field theory, fields are replaced by superfields, which contain bothbosons and fermions
field→ superfield =
(boson
fermion
)
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable,
and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
The Minimal Supersymmetric Standard Model
MSSM = Standard Model + supersymmetry
It is described by the superpotential
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
There are new superparticles for each of the Standard Model particles. For example
quark→(
squarkquark
)spin 0spin 1
2
, photon→(
photinophoton
)spin 1
2spin 1
The lightest superparticle (LSP) is expected to be stable, and is usually assumed to bea neutralino, which is a mixture of the Higgsino, photino and Zino.
Physical motivation
I In the Standard Model, the mass of the Higgs boson is quantum mechanicallyunstable. Supersymmetry stabilizes the Higgs boson’s mass.
I The MSSM leads to gauge coupling unification, and hence by assuming gaugecoupling unification can correctly predict one of the gauge couplings from theother two.
For these reasons, supersymmetry, in the form of the MSSM, is expected to bediscovered next year!
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
tau
muon
electron
neutrinos
top
bottomcharm
strange
downup
Higgs
photon
Z W
gluon
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
gluino
gluon
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
graviton
The strong CP problem
The strong interactions would be expected to contain a CP violating term
θF ∧ F
where F is the gluon field strength.
However, experimental constraints on the electricdipole moment of the neutron require
θ . 10−10
The strong CP problem
The strong interactions would be expected to contain a CP violating term
θF ∧ F
where F is the gluon field strength. However, experimental constraints on the electricdipole moment of the neutron require
θ . 10−10
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F →(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion. The minima of the axionpotential are automatically CP conserving, cancelling off the problematic term.
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)
If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F →(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion. The minima of the axionpotential are automatically CP conserving, cancelling off the problematic term.
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F
→(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion. The minima of the axionpotential are automatically CP conserving, cancelling off the problematic term.
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F →(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion. The minima of the axionpotential are automatically CP conserving, cancelling off the problematic term.
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F →
(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion.
The minima of the axionpotential are automatically CP conserving, cancelling off the problematic term.
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F →
(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion.
The minima of the axionpotential are automatically CP conserving, cancelling off the problematic term.
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F →
(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion. The minima of the axionpotential are automatically CP conserving,
cancelling off the problematic term.
Axions
The strong CP problem can be solved by introducing a complex scalar field φ with arotationally symmetric classical potential
axion
CP conserving vacua
The angular part of the field is the axion
φ = φ0 exp
(ia√
2φ0
)If φ is coupled to quarks, then the parameter θ becomes dynamical
θF ∧ F →
(θ −
Na√
2φ0
)F ∧ F
and quantum mechanics generates a potential for the axion. The minima of the axionpotential are automatically CP conserving, cancelling off the problematic term.
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
axion
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
graviton
Gravitinos
graviton→(
gravitinograviton
)spin 3
2spin 2
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion Gravity
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion Gravity
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
gravitino
graviton
Moduli
field theories → many arbitrary parameters
string theory → no parameters
many scalar fields (moduli)
moduli vacuum values → low energy parameters
Typically moduli have Planckian values and so gravitational strength interactions.This makes them relatively long lived
moduli half-life ∼ minutes
Moduli
field theories → many arbitrary parameters
string theory → many scalar fields (moduli)
moduli vacuum values → low energy parameters
Typically moduli have Planckian values and so gravitational strength interactions.This makes them relatively long lived
moduli half-life ∼ minutes
Moduli
field theories → many arbitrary parameters
string theory → many scalar fields (moduli)
moduli vacuum values → low energy parameters
Typically moduli have Planckian values and so gravitational strength interactions.This makes them relatively long lived
moduli half-life ∼ minutes
Moduli
field theories → many arbitrary parameters
string theory → many scalar fields (moduli)
moduli vacuum values → low energy parameters
Typically moduli have Planckian values and so gravitational strength interactions.This makes them relatively long lived
moduli half-life ∼ minutes
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion Gravity
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
gravitino
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion Gravity
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
modulinosmoduli gravitino
graviton
Particle spectrum
electron
neutronproton
photon graviton
Particle spectrum
Quarks Strong
electron
top
bottomcharm
strange
downup
photon
gluon
graviton
Particle spectrum
Leptons Quarks Electroweak Strong
tau
muon
electron
neutrinos
top
bottomcharm
strange
downup
photon
Z W
gluon
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
tau
muon
electron
neutrinos
top
bottomcharm
strange
downup
Higgs
photon
Z W
gluon
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
graviton
Particle spectrum
Leptons Quarks Higgs Electroweak Strong Axion Gravity
sleptons
tau
muon
electron
neutrinos
squarks
top
bottomcharm
strange
downup
Higgsino
Higgs
photino
photon
Zino
Z
Wino
W
neutralinogluino
gluon
saxino
axino
axion
modulinosmoduli gravitino
graviton
The Origin of Matter
The Standard ModelOrdinary matterQuarksNeutrinosHiggs boson
Beyond the Standard ModelNeutrino massesSupersymmetryAxionsGravitinos and moduliParticle spectrum
Big Bang cosmologyThe hot Big BangPrimordial inflationMatter/antimatter asymmetryDark matterGravitinos and moduli
A theory for the origin of matterA Minimal Supersymmetric Cosmological ModelThermal inflationBaryogenesisDark matterHistory of the observable universe
The hot Big Bang
Big Bang = hot dense universe expands and cools
Based on General Relativity, the observed Hubble expansion and three keyobservationally verified theories:
Nucleosynthesis T ∼ 0.1 MeV
protons + neutrons→ 4He, 2H, 3He, 7Li , . . .
Microwave background T ∼ 0.3 eV
plasma→ atoms + photons
Galaxy formation T ∼ 1 eV
radiation domination→ matter domination
T . 1 eVdensity perturbations→ galaxies . . .
The hot Big Bang
Big Bang = hot dense universe expands and cools
Based on General Relativity, the observed Hubble expansion and three keyobservationally verified theories:
Nucleosynthesis T ∼ 0.1 MeV
protons + neutrons→ 4He, 2H, 3He, 7Li , . . .
Microwave background T ∼ 0.3 eV
plasma→ atoms + photons
Galaxy formation T ∼ 1 eV
radiation domination→ matter domination
T . 1 eVdensity perturbations→ galaxies . . .
The hot Big Bang
Big Bang = hot dense universe expands and cools
Based on General Relativity, the observed Hubble expansion and three keyobservationally verified theories:
Nucleosynthesis T ∼ 0.1 MeV
protons + neutrons→ 4He, 2H, 3He, 7Li , . . .
Microwave background T ∼ 0.3 eV
plasma→ atoms + photons
Galaxy formation T ∼ 1 eV
radiation domination→ matter domination
T . 1 eVdensity perturbations→ galaxies . . .
The hot Big Bang
Big Bang = hot dense universe expands and cools
Based on General Relativity, the observed Hubble expansion and three keyobservationally verified theories:
Nucleosynthesis T ∼ 0.1 MeV
protons + neutrons→ 4He, 2H, 3He, 7Li , . . .
Microwave background T ∼ 0.3 eV
plasma→ atoms + photons
Galaxy formation T ∼ 1 eV
radiation domination→ matter domination
T . 1 eVdensity perturbations→ galaxies . . .
The hot Big Bang
Big Bang = hot dense universe expands and cools
Based on General Relativity, the observed Hubble expansion and three keyobservationally verified theories:
Nucleosynthesis T ∼ 0.1 MeV
protons + neutrons→ 4He, 2H, 3He, 7Li , . . .
Microwave background T ∼ 0.3 eV
plasma→ atoms + photons
Galaxy formation T ∼ 1 eV
radiation domination→ matter domination
T . 1 eVdensity perturbations→ galaxies . . .
History of the observable universe
RADIATION
MATTER
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
Vacuum energy
field0
potential
vacuaparticles
vacuum energy density
Figure: What is a vacuum?
vacuummore vacuummore vacuum energy
Figure: What happens when you expand a vacuum?
Vacuum energy
field0
potential
vacua
particles
vacuum energy density
Figure: What is a vacuum?
vacuummore vacuummore vacuum energy
Figure: What happens when you expand a vacuum?
Vacuum energy
field0
potential
vacua
particles
vacuum energy density
Figure: What is a vacuum?
vacuummore vacuummore vacuum energy
Figure: What happens when you expand a vacuum?
Vacuum energy
field0
potential
vacua
particles
vacuum energy density
Figure: What is a vacuum?
vacuummore vacuummore vacuum energy
Figure: What happens when you expand a vacuum?
Vacuum energy
field0
potential
vacua
particles
vacuum energy density
Figure: What is a vacuum?
vacuum
more vacuummore vacuum energy
Figure: What happens when you expand a vacuum?
Vacuum energy
field0
potential
vacua
particles
vacuum energy density
Figure: What is a vacuum?
vacuum
more vacuum
more vacuum energy
Figure: What happens when you expand a vacuum?
Vacuum energy
field0
potential
vacua
particles
vacuum energy density
Figure: What is a vacuum?
vacuummore vacuum
more vacuum energy
Figure: What happens when you expand a vacuum?
Inflation
VACUUMENERGY
VACUUMENERGY
VACUUMENERGY
Figure: What happens if the expanding universe has positive vacuum energy?
Inflation
VACUUMENERGY
VACUUMENERGY
VACUUMENERGY
Figure: What happens if the expanding universe has positive vacuum energy?
Inflation
VACUUMENERGY
VACUUMENERGY
VACUUMENERGY
Figure: What happens if the expanding universe has positive vacuum energy?
Primordial inflation
inflation→{
vacuum cleans the universegenerates vast amounts of energy
vacuum energy decays→ hot Big Bang
Furthermore
quantumvacuum
fluctuations
inflation−→classicaldensity
perturbations
gravity−→ galaxies . . .
Primordial inflation
inflation→{
vacuum cleans the universegenerates vast amounts of energy
vacuum energy decays→ hot Big Bang
Furthermore
quantumvacuum
fluctuations
inflation−→classicaldensity
perturbations
gravity−→ galaxies . . .
Primordial inflation
inflation→{
vacuum cleans the universegenerates vast amounts of energy
vacuum energy decays→ hot Big Bang
Furthermore
quantumvacuum
fluctuations
inflation−→classicaldensity
perturbations
gravity−→ galaxies . . .
Primordial inflation
inflation→{
vacuum cleans the universegenerates vast amounts of energy
vacuum energy decays→ hot Big Bang
Furthermore
quantumvacuum
fluctuations
inflation−→classicaldensity
perturbations
gravity−→ galaxies . . .
Primordial inflation
inflation→{
vacuum cleans the universegenerates vast amounts of energy
vacuum energy decays→ hot Big Bang
Furthermore
quantumvacuum
fluctuations
inflation−→classicaldensity
perturbations
gravity−→ galaxies . . .
History of the observable universe
RADIATION
MATTER
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
Matter and antimatter
Every particle has an antiparticle with equal mass and opposite charges
electron ↔ antielectron
quark ↔ antiquark
photon ↔ photon
Particle-antiparticle pairs are created from, and annihilate into, pure energy
matter + antimatter = energy
In the early universe
inflation→ energy→ matter + antimatter
but now only matter is left. Why?If a small matter/antimatter asymmetry, with slightly more matter than antimatter,can be generated (baryogenesis) then
matter/antimatterasymmetry
annihilation−→ matter
Matter and antimatter
Every particle has an antiparticle with equal mass and opposite charges
electron ↔ antielectron
quark ↔ antiquark
photon ↔ photon
Particle-antiparticle pairs are created from, and annihilate into, pure energy
matter + antimatter = energy
In the early universe
inflation→ energy→ matter + antimatter
but now only matter is left. Why?If a small matter/antimatter asymmetry, with slightly more matter than antimatter,can be generated (baryogenesis) then
matter/antimatterasymmetry
annihilation−→ matter
Matter and antimatter
Every particle has an antiparticle with equal mass and opposite charges
electron ↔ antielectron
quark ↔ antiquark
photon ↔ photon
Particle-antiparticle pairs are created from, and annihilate into, pure energy
matter + antimatter = energy
In the early universe
inflation→ energy→ matter + antimatter
but now only matter is left. Why?If a small matter/antimatter asymmetry, with slightly more matter than antimatter,can be generated (baryogenesis) then
matter/antimatterasymmetry
annihilation−→ matter
Matter and antimatter
Every particle has an antiparticle with equal mass and opposite charges
electron ↔ antielectron
quark ↔ antiquark
photon ↔ photon
Particle-antiparticle pairs are created from, and annihilate into, pure energy
matter + antimatter = energy
In the early universe
inflation→ energy→ matter + antimatter
but now only matter is left. Why?
If a small matter/antimatter asymmetry, with slightly more matter than antimatter,can be generated (baryogenesis) then
matter/antimatterasymmetry
annihilation−→ matter
Matter and antimatter
Every particle has an antiparticle with equal mass and opposite charges
electron ↔ antielectron
quark ↔ antiquark
photon ↔ photon
Particle-antiparticle pairs are created from, and annihilate into, pure energy
matter + antimatter = energy
In the early universe
inflation→ energy→ matter + antimatter
but now only matter is left. Why?If a small matter/antimatter asymmetry, with slightly more matter than antimatter,can be generated (baryogenesis) then
matter/antimatterasymmetry
annihilation−→ matter
Baryogenesis mechanisms
Particle decayheavy particles
out of equilibriumdecay−→ matter/antimatter
asymmetry
Best example is decay of right-handed neutrinos.
Electroweak phase transition If the electroweak phase transition is first order
expandingbubble walls
→ matter/antimatterasymmetry
Affleck-Dine baryogenesis
angular momentumin field space
=matter/antimatter
asymmetry
Baryogenesis mechanisms
Particle decayheavy particles
out of equilibriumdecay−→ matter/antimatter
asymmetry
Best example is decay of right-handed neutrinos.
Electroweak phase transition If the electroweak phase transition is first order
expandingbubble walls
→ matter/antimatterasymmetry
Affleck-Dine baryogenesis
angular momentumin field space
=matter/antimatter
asymmetry
Baryogenesis mechanisms
Particle decayheavy particles
out of equilibriumdecay−→ matter/antimatter
asymmetry
Best example is decay of right-handed neutrinos.
Electroweak phase transition If the electroweak phase transition is first order
expandingbubble walls
→ matter/antimatterasymmetry
Affleck-Dine baryogenesis
angular momentumin field space
=matter/antimatter
asymmetry
Baryogenesis mechanisms
Particle decayheavy particles
out of equilibriumdecay−→ matter/antimatter
asymmetry
Best example is decay of right-handed neutrinos.
Electroweak phase transition If the electroweak phase transition is first order
expandingbubble walls
→ matter/antimatterasymmetry
Affleck-Dine baryogenesis
angular momentumin field space
=matter/antimatter
asymmetry
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
electroweak transition matter/antimatter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
Dark matter
Two good candidates
Neutralino The neutralino is usually assumed to be the lightest superparticle(LSP) and hence stable. It is left as a remnant of the hot earlyuniverse.
Axion Generated in coherent oscillations when the axion potential turns onduring the QCD phase transition (when the strong nuclear forcebecomes strong).
Dark matter
Two good candidates
Neutralino The neutralino is usually assumed to be the lightest superparticle(LSP) and hence stable. It is left as a remnant of the hot earlyuniverse.
Axion Generated in coherent oscillations when the axion potential turns onduring the QCD phase transition (when the strong nuclear forcebecomes strong).
Dark matter
Two good candidates
Neutralino The neutralino is usually assumed to be the lightest superparticle(LSP) and hence stable. It is left as a remnant of the hot earlyuniverse.
Axion Generated in coherent oscillations when the axion potential turns onduring the QCD phase transition (when the strong nuclear forcebecomes strong).
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
electroweak transition matter/antimatter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
electroweak transition matter/antimatter?neutralino freeze out neutralino dark matter?
QCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
Gravitinos and moduli
Moduli (scalar fields with Planckian vacuum values) are cosmologically dangerous. Forexample, nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Gravitinos are thermally produced in the early universe, leading to a similar, thoughless severe, problem.
Gravitinos and moduli
Moduli (scalar fields with Planckian vacuum values) are cosmologically dangerous. Forexample, nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Gravitinos are thermally produced in the early universe, leading to a similar, thoughless severe, problem.
Gravitinos and moduli
Moduli (scalar fields with Planckian vacuum values) are cosmologically dangerous. Forexample, nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Gravitinos are thermally produced in the early universe, leading to a similar, thoughless severe, problem.
Gravitinos and moduli
Moduli (scalar fields with Planckian vacuum values) are cosmologically dangerous. Forexample, nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Gravitinos are thermally produced in the early universe, leading to a similar, thoughless severe, problem.
Gravitinos and moduli
Moduli (scalar fields with Planckian vacuum values) are cosmologically dangerous. Forexample, nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Gravitinos are thermally produced in the early universe, leading to a similar, thoughless severe, problem.
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
electroweak transition matter/antimatter?neutralino freeze out neutralino dark matter?
QCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
moduli, gravitinos, . . . disaster
electroweak transition matter/antimatter?neutralino freeze out neutralino dark matter?
QCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
The Origin of Matter
The Standard ModelOrdinary matterQuarksNeutrinosHiggs boson
Beyond the Standard ModelNeutrino massesSupersymmetryAxionsGravitinos and moduliParticle spectrum
Big Bang cosmologyThe hot Big BangPrimordial inflationMatter/antimatter asymmetryDark matterGravitinos and moduli
A theory for the origin of matterA Minimal Supersymmetric Cosmological ModelThermal inflationBaryogenesisDark matterHistory of the observable universe
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term axion
thermal inflationbaryogenesis dark matter
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM
neutrino masses MSSM µ-term axion
thermal inflationbaryogenesis dark matter
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses
MSSM µ-term axion
thermal inflationbaryogenesis dark matter
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term
axion
thermal inflationbaryogenesis dark matter
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term axion
thermal inflationbaryogenesis dark matter
Thermal inflation
The superpotential termW = λχφχχ
generates a potential
V = V0 −m2φ|φ|
2+m2χ|χ|2+m2
χ|χ|2+[Aχλχφχχ+ c.c.]+ |λχχφ|2 + |λχχφ|2+|λχχχ|2
At finite temperature
V (φ) = V0
+g2T 2|φ|2
−m2φ|φ|
2 + . . .
T & mφ =⇒ φ = 0
T 4 . V0 =⇒ inflation
Thermal inflation
The superpotential termW = λχφχχ
generates a potential
V = V0 −m2φ|φ|
2+m2χ|χ|2+m2
χ|χ|2+[Aχλχφχχ+ c.c.]+ |λχχφ|2 + |λχχφ|2+|λχχχ|2
At finite temperature
V (φ) = V0
+g2T 2|φ|2
−m2φ|φ|
2 + . . .
T & mφ =⇒ φ = 0
T 4 . V0 =⇒ inflation
Thermal inflation
The superpotential termW = λχφχχ
generates a potential
V = V0 −m2φ|φ|
2+m2χ|χ|2+m2
χ|χ|2+[Aχλχφχχ+ c.c.]+ |λχχφ|2 + |λχχφ|2+|λχχχ|2
At finite temperature
V (φ) = V0+g2T 2|φ|2−m2φ|φ|
2 + . . .
T & mφ =⇒ φ = 0
T 4 . V0 =⇒ inflation
Thermal inflation
The superpotential termW = λχφχχ
generates a potential
V = V0 −m2φ|φ|
2+m2χ|χ|2+m2
χ|χ|2+[Aχλχφχχ+ c.c.]+ |λχχφ|2 + |λχχφ|2+|λχχχ|2
At finite temperature
V (φ) = V0+g2T 2|φ|2−m2φ|φ|
2 + . . .
T & mφ =⇒ φ = 0
T 4 . V0 =⇒ inflation
Thermal inflation
The superpotential termW = λχφχχ
generates a potential
V = V0 −m2φ|φ|
2+m2χ|χ|2+m2
χ|χ|2+[Aχλχφχχ+ c.c.]+ |λχχφ|2 + |λχχφ|2+|λχχχ|2
At finite temperature
V (φ) = V0+g2T 2|φ|2−m2φ|φ|
2 + . . .
T & mφ =⇒ φ = 0
T 4 . V0 =⇒ inflation
Thermal inflation
|φ|
V
φ0
V0
Figure: Radiation domination
Thermal inflation
|φ|
V
φ0
V0
Figure: Thermal inflation
Thermal inflation
|φ|
V
φ0
V0
Figure: Thermal inflation
Thermal inflation
|φ|
V
φ0
V0
Figure: First order phase transition
Thermal inflation
|φ|
V
φ0
V0
Figure: Potential energy converted to particles
Thermal inflation
|φ|
V
φ0
V0
Figure: Matter domination
Key properties of thermal inflation
ForV
1/40 ∼ 106 to 107 GeV
Dilution factor (1020): pre-existing moduli sufficiently diluted.
Low energy scale (H ∼ 10−8m): moduli regenerated with sufficiently smallabundance.
Short duration (N ∼ 10): density perturbations from primordial inflation preserved onlarge scales.
Key properties of thermal inflation
ForV
1/40 ∼ 106 to 107 GeV
Dilution factor (1020): pre-existing moduli sufficiently diluted.
Low energy scale (H ∼ 10−8m): moduli regenerated with sufficiently smallabundance.
Short duration (N ∼ 10): density perturbations from primordial inflation preserved onlarge scales.
Key properties of thermal inflation
ForV
1/40 ∼ 106 to 107 GeV
Dilution factor (1020): pre-existing moduli sufficiently diluted.
Low energy scale (H ∼ 10−8m): moduli regenerated with sufficiently smallabundance.
Short duration (N ∼ 10): density perturbations from primordial inflation preserved onlarge scales.
Key properties of thermal inflation
ForV
1/40 ∼ 106 to 107 GeV
Dilution factor (1020): pre-existing moduli sufficiently diluted.
Low energy scale (H ∼ 10−8m): moduli regenerated with sufficiently smallabundance.
Short duration (N ∼ 10): density perturbations from primordial inflation preserved onlarge scales.
Gravitational waves from thermal inflation
The comoving length scale of thermal inflation is of order the Earth-Moon system. Onthese scales:
I any gravitational waves from primordial inflation wiped out
I new gravitational waves generated by the first order phase transition at the end ofthermal inflation
May be observable at future space based gravitational wave detectors such as BBO orDECIGO.
Gravitational waves from thermal inflation
The comoving length scale of thermal inflation is of order the Earth-Moon system. Onthese scales:
I any gravitational waves from primordial inflation wiped out
I new gravitational waves generated by the first order phase transition at the end ofthermal inflation
May be observable at future space based gravitational wave detectors such as BBO orDECIGO.
Gravitational waves from thermal inflation
The comoving length scale of thermal inflation is of order the Earth-Moon system. Onthese scales:
I any gravitational waves from primordial inflation wiped out
I new gravitational waves generated by the first order phase transition at the end ofthermal inflation
May be observable at future space based gravitational wave detectors such as BBO orDECIGO.
Gravitational waves from thermal inflation
The comoving length scale of thermal inflation is of order the Earth-Moon system. Onthese scales:
I any gravitational waves from primordial inflation wiped out
I new gravitational waves generated by the first order phase transition at the end ofthermal inflation
May be observable at future space based gravitational wave detectors such as BBO orDECIGO.
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
moduli, gravitinos, . . . disaster
electroweak transition matter/antimatter?neutralino freeze out neutralino dark matter?
QCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational waves
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
Baryogenesis
Key assumption
m2LHu
=1
2
(m2
L + m2Hu
)< 0
Implies a dangerous non-MSSM vacuum with LHu ∼ (109GeV)2 and
λdQLd + λeLLe = µLHu
eliminating the µ-term contribution to LHu ’s mass squared.
LHu ,QLd , LLe
V
0
our vacuum
another vacuum
Baryogenesis
Key assumption
m2LHu
=1
2
(m2
L + m2Hu
)< 0
Implies a dangerous non-MSSM vacuum with LHu ∼ (109GeV)2 and
λdQLd + λeLLe = µLHu
eliminating the µ-term contribution to LHu ’s mass squared.
LHu ,QLd , LLe
V
0
our vacuum
another vacuum
Reduction
L =
(l0
), Hu =
(0hu
), Hd =
(hd
0
), e =
(0)
u =(
0 0 0)
, Q =
(0 0 0
d/√
2 0 0
), d =
(d/√
2 0 0)
φ = φ , χ = 0 , χ = 0
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced outd held at origin
lhu returnswith
rotation
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation
lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced outd held at origin
lhu returnswith
rotation
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced outd held at origin
lhu returnswith
rotation
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced outd held at origin
lhu returnswith
rotation
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced outd held at origin
lhu returnswith
rotation
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d held at origin
lhu returnswith
rotation
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced outd held at origin
lhu returnswith
rotation
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 +
1
2
(m2
Q + m2d
)|d |2 − m2
φ|φ|2
+
[1
2Aνλν l
2h2u −
1
2Adλdhdd2 − Aµλµφ
2huhd + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2
∣∣∣∣2+ |λdhdd |2 + |2λµφhuhd |2 +
1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2
)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced outd held at origin
lhu returnswith
rotation
Baryogenesis
MODULIDOMINATION
THERMALINFLATION
FLATONDOMINATION
RADIATIONDOMINATION
φ = 0
φ > 0
φ ∼ φ0
φ preheats
φ decays
huhd = 0
hd > 0 ⇒ d = e = 0
lhu = 0
lhu > 0
brought back into origin with rotation⇒ nL < 0
preheating and thermal friction⇒ NL conserved
l , hu , hd decayT > TEW ⇒ nL → nB
dilution ⇒ nB/s ∼ 10−10
nucleosynthesis
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational waves
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
Dark matter
A mixture of
Axino The axino is the lightest superparticle (LSP) and hence stable. It isgenerated by the decay of the saxino, and by the decay of the nextlightest superparticle (NLSP).
Axion As before, generated in coherent oscillations when the axionpotential turns on during the QCD phase transition, though may bediluted by the decay of the saxino.
thermal inflation
saxinomatter domination
radiationdominationaxinos axions
firstorder
phasetransition
decaydecay
NLSP
decay
QCD phase
transition
Axino LHC signal
Next lightest superparticles (NLSPs) produced by the Large Hadron Collider (LHC)decay to axinos plus Standard Model particles
LHCNLSP
axino
SM102 m
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
saxino decay axino dark matterQCD transition axion dark matter
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
saxino decay axino dark matterQCD transition axion dark matter
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term axion
thermal inflationbaryogenesis dark matter
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term axion
thermal inflation
baryogenesis dark matter
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term axion
thermal inflationbaryogenesis
dark matter
A Minimal Supersymmetric Cosmological Model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term axion
thermal inflationbaryogenesis dark matter
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
electroweak transition matter/antimatter?neutralino freeze out neutralino dark matter?
QCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
right-handed neutrino decay matter/antimatter?
moduli, gravitinos, . . . disaster
electroweak transition matter/antimatter?neutralino freeze out neutralino dark matter?
QCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational waves
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
saxino decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
saxino decay axino dark matterQCD transition axion dark matter
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
History of the observable universe
(density)1/4
time
mPl
1011 GeV
103 GeV
100 keV
10 K
tPl
10−28 s
10−13 s
10 min
1010 yr
inflationdensity perturbationsgravitational waves?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
saxino decay axino dark matterQCD transition axion dark matter
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
The Origin of Matter
The Standard ModelOrdinary matterQuarksNeutrinosHiggs boson
Beyond the Standard ModelNeutrino massesSupersymmetryAxionsGravitinos and moduliParticle spectrum
Big Bang cosmologyThe hot Big BangPrimordial inflationMatter/antimatter asymmetryDark matterGravitinos and moduli
A theory for the origin of matterA Minimal Supersymmetric Cosmological ModelThermal inflationBaryogenesisDark matterHistory of the observable universe
