The Origin of Matter - profstewart.orgprofstewart.org/papers/matter.pdf · 2013-01-23 · The Origin of Matter The Standard Model Ordinary matter Quarks Neutrinos Higgs boson Beyond

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