a minimal supersymmetric cosmological model - …profstewart.org/papers/beyond2010_stewart.pdf · a...
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![Page 1: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/1.jpg)
A Minimal Supersymmetric Cosmological Model
Ewan Stewart
KAIST
Beyond the Standard Models ofParticle Physics, Cosmology and Astrophysics
2 February 2010Cape Town, South Africa
Donghui Jeong, Kenji Kadota, Wan-Il Park, EDS hep-ph/0406136Gary N Felder, Hyunbyuk Kim, Wan-Il Park, EDS hep-ph/0703275
Richard Easther, John T Giblin, Eugene A Lim, Wan-Il Park, EDS arXiv:0801.4197Seongcheol Kim, Wan-Il Park, EDS arXiv:0807.3607
![Page 2: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/2.jpg)
A Minimal Supersymmetric Cosmological Model
Ewan Stewart
KAIST
Beyond the Standard Models ofParticle Physics, Cosmology and Astrophysics
2 February 2010Cape Town, South Africa
Donghui Jeong, Kenji Kadota, Wan-Il Park, EDS hep-ph/0406136Gary N Felder, Hyunbyuk Kim, Wan-Il Park, EDS hep-ph/0703275
Richard Easther, John T Giblin, Eugene A Lim, Wan-Il Park, EDS arXiv:0801.4197Seongcheol Kim, Wan-Il Park, EDS arXiv:0807.3607
![Page 3: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/3.jpg)
Standard model of cosmology
(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?
νR 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
![Page 4: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/4.jpg)
Moduli and gravitinos
Moduli are cosmologically dangerous. Nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Moduli generated: H . msusy
after
slow-roll inflation: H & minflaton & msusy
![Page 5: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/5.jpg)
Moduli and gravitinos
Moduli are cosmologically dangerous. Nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Moduli generated: H . msusy
after
slow-roll inflation: H & minflaton & msusy
![Page 6: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/6.jpg)
Moduli and gravitinos
Moduli are cosmologically dangerous. Nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Moduli generated: H . msusy
after
slow-roll inflation: H & minflaton & msusy
![Page 7: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/7.jpg)
Moduli and gravitinos
Moduli are cosmologically dangerous. Nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Moduli generated: H . msusy
after
slow-roll inflation: H & minflaton & msusy
![Page 8: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/8.jpg)
Moduli and gravitinos
Moduli are cosmologically dangerous. Nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Moduli generated: H . msusy
after
slow-roll inflation: H & minflaton & msusy
![Page 9: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/9.jpg)
Moduli and gravitinos
Moduli are cosmologically dangerous. Nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Moduli generated: H . msusy
after
slow-roll inflation: H & minflaton & msusy
![Page 10: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/10.jpg)
Moduli and gravitinos
Moduli are cosmologically dangerous. Nucleosynthesis constrains
n
s. 10−12
In the early universe
H2 (Ψ−Ψ1)2
m2susy (Ψ−Ψ0)2
∼ MPl
n
s∼ 107
Moduli generated: H . msusy
after
slow-roll inflation: H & minflaton & msusy
![Page 11: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/11.jpg)
Standard model of cosmology
(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?
νR 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
![Page 12: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/12.jpg)
Standard model of cosmology
(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?
νR 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
![Page 13: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/13.jpg)
Minimal Supersymmetric Standard Model
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
But
I µ?
I neutrino masses?
I strong CP?
![Page 14: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/14.jpg)
Minimal Supersymmetric Standard Model
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
But
I µ?
I neutrino masses?
I strong CP?
![Page 15: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/15.jpg)
Minimal Supersymmetric Standard Model
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
But
I µ?
I neutrino masses?
I strong CP?
![Page 16: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/16.jpg)
Minimal Supersymmetric Standard Model
W = λuQHu u + λdQHd d + λeLHd e + µHuHd
But
I µ?
I neutrino masses?
I strong CP?
![Page 17: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/17.jpg)
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 drives m2φ < 0
axion
µ = λµφ20
|φ|
V
φ0
V0
![Page 18: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/18.jpg)
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 drives m2φ < 0
axion
µ = λµφ20
|φ|
V
φ0
V0
![Page 19: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/19.jpg)
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 drives m2φ < 0
axion
µ = λµφ20
|φ|
V
φ0
V0
![Page 20: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/20.jpg)
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
drives m2φ < 0
axion
µ = λµφ20
|φ|
V
φ0
V0
![Page 21: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/21.jpg)
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 drives m2φ < 0
axion
µ = λµφ20
|φ|
V
φ0
V0
![Page 22: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/22.jpg)
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 drives m2φ < 0
axion
µ = λµφ20
|φ|
V
φ0
V0
![Page 23: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/23.jpg)
Thermal inflation
|φ|
V
φ0
V0
RADIATIONDOMINATION
![Page 24: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/24.jpg)
Thermal inflation
|φ|
V
φ0
V0
THERMALINFLATION
![Page 25: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/25.jpg)
Thermal inflation
|φ|
V
φ0
V0
THERMALINFLATION
![Page 26: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/26.jpg)
Thermal inflation
|φ|
V
φ0
V0
first orderphase transition
![Page 27: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/27.jpg)
Thermal inflation
|φ|
V
φ0
V0
potential energyconverted to
particles
![Page 28: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/28.jpg)
Thermal inflation
|φ|
V
φ0
V0
MATTERDOMINATION
![Page 29: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/29.jpg)
Key properties of thermal inflation
Forφ0 ∼ 1010 to 1012 GeV
Large dilution
∆ ∼ 1020 =⇒ pre-existing moduli sufficiently diluted
Short duration
N ∼ 10 =⇒primordial perturbationsfrom slow-roll inflation
preserved on large scales
Low energy scale
V1/40 ∼ 106 to 107 GeV =⇒ moduli regenerated with
sufficiently small abundance
![Page 30: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/30.jpg)
Key properties of thermal inflation
Forφ0 ∼ 1010 to 1012 GeV
Large dilution
∆ ∼ 1020 =⇒ pre-existing moduli sufficiently diluted
Short duration
N ∼ 10 =⇒primordial perturbationsfrom slow-roll inflation
preserved on large scales
Low energy scale
V1/40 ∼ 106 to 107 GeV =⇒ moduli regenerated with
sufficiently small abundance
![Page 31: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/31.jpg)
Key properties of thermal inflation
Forφ0 ∼ 1010 to 1012 GeV
Large dilution
∆ ∼ 1020 =⇒ pre-existing moduli sufficiently diluted
Short duration
N ∼ 10 =⇒primordial perturbationsfrom slow-roll inflation
preserved on large scales
Low energy scale
V1/40 ∼ 106 to 107 GeV =⇒ moduli regenerated with
sufficiently small abundance
![Page 32: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/32.jpg)
Key properties of thermal inflation
Forφ0 ∼ 1010 to 1012 GeV
Large dilution
∆ ∼ 1020 =⇒ pre-existing moduli sufficiently diluted
Short duration
N ∼ 10 =⇒primordial perturbationsfrom slow-roll inflation
preserved on large scales
Low energy scale
V1/40 ∼ 106 to 107 GeV =⇒ moduli regenerated with
sufficiently small abundance
![Page 33: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/33.jpg)
Gravitational waves
f
Hz
ΩGW
10−10 10−5 100 105 101010−40
10−35
10−30
10−25
10−20
10−15
10−10
10−5
PRIMORDIALINFLATION
INFLATIONPREHEATING
DECIGO
array
![Page 34: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/34.jpg)
Gravitational waves
f
Hz
ΩGW
10−10 10−5 100 105 101010−40
10−35
10−30
10−25
10−20
10−15
10−10
10−5
PRIMORDIALINFLATION
INFLATIONPREHEATING
THERMAL
INFLATION
DECIGO
array
![Page 35: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/35.jpg)
Baryogenesis
Key assumption
m2LHu
=1
2
(m2
L + m2Hu
)< 0
Implies a dangerous non-MSSM vacuum with
LHu ∼ (109GeV)2
andλdQLd + λeLLe = µLHu
eliminating the µ-term contribution to LHu ’s mass squared.
LHu ,QLd , LLe
V
0
our vacuum
deeper vacuum
![Page 36: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/36.jpg)
Baryogenesis
Key assumption
m2LHu
=1
2
(m2
L + m2Hu
)< 0
Implies a dangerous non-MSSM vacuum with
LHu ∼ (109GeV)2
andλdQLd + λeLLe = µLHu
eliminating the µ-term contribution to LHu ’s mass squared.
LHu ,QLd , LLe
V
0
our vacuum
deeper vacuum
![Page 37: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/37.jpg)
Reduction
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2HuHd + λχφχχ
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
![Page 38: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/38.jpg)
Reduction
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2HuHd + λχφχχ
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
![Page 39: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/39.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 40: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/40.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation
lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 41: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/41.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 42: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/42.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 43: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/43.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 44: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/44.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 45: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/45.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 46: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/46.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 − m2
φ|φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 47: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/47.jpg)
Potential
V = V0 + m2L|l |
2 −m2Hu|hu |2 + m2
Hd|hd |2 + m2
φ(φ) |φ|2
+1
2
(m2
Q + m2d
)|d |2 +
1
2
(m2
L + m2e
)|e|2
+
[1
2Aνλν l
2h2u − Aµλµφ
2huhd −1
2Adλdhdd2 +
1
2Aeλehde2 + c.c.
]+∣∣λν lh2
u
∣∣2 +∣∣∣λν l2hu − λµφ2hd
∣∣∣2 +
∣∣∣∣λµφ2hu +1
2λdd2 +
1
2λee
2
∣∣∣∣2+ |λdhdd |2 + |λehde|2 + |2λµφhuhd |2
+1
2g2
(|hu |2 − |hd |2 − |l |2 +
1
2|d |2 +
1
2|e|2)2
drives thermal inflation lhu rolls away
lhu stabilizedwith
fixed phase
φ rolls away
hd forced out
d and e held at origin
lhu returnswith
rotation
φ stabilizedm2φ(φ0) = −αφm2
φ(0)
![Page 48: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/48.jpg)
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
![Page 49: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/49.jpg)
Numerical simulation
mt
nL/nAD
0 200 400 600 800 1000−0.15
−0.1
−0.05
0
0.05
0.1
0.15
![Page 50: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/50.jpg)
Baryon asymmetry
nB
s∼
nL
nAD
nAD
nφ
Td
mφ(φ0)
Usingnφ ∼ mφ(φ0)φ2
0 , m2φ(φ0) ∼ αφm2
φ(0) , nAD ∼ mLHu l20
l0 ∼ 109 GeV
√(10−2 eV
mν
)( mLHu
103 GeV
)and
Td ∼ 1 GeV
(1012 GeV
φ0
)(|µ|
103 GeV
)2
gives
nB
s∼ 10−10
(nL/nAD
10−2
)(1012 GeV
φ0
)3 (10−2 eV
mν
)(|µ|
103 GeV
)2 (10−1
αφ
)(mLHu
mφ(0)
)2
which suggestsφ0 ∼ 1012 GeV
![Page 51: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/51.jpg)
Baryon asymmetry
nB
s∼
nL
nAD
nAD
nφ
Td
mφ(φ0)
Usingnφ ∼ mφ(φ0)φ2
0 , m2φ(φ0) ∼ αφm2
φ(0) , nAD ∼ mLHu l20
l0 ∼ 109 GeV
√(10−2 eV
mν
)( mLHu
103 GeV
)and
Td ∼ 1 GeV
(1012 GeV
φ0
)(|µ|
103 GeV
)2
gives
nB
s∼ 10−10
(nL/nAD
10−2
)(1012 GeV
φ0
)3 (10−2 eV
mν
)(|µ|
103 GeV
)2 (10−1
αφ
)(mLHu
mφ(0)
)2
which suggestsφ0 ∼ 1012 GeV
![Page 52: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/52.jpg)
Baryon asymmetry
nB
s∼
nL
nAD
nAD
nφ
Td
mφ(φ0)
Usingnφ ∼ mφ(φ0)φ2
0 , m2φ(φ0) ∼ αφm2
φ(0) , nAD ∼ mLHu l20
l0 ∼ 109 GeV
√(10−2 eV
mν
)( mLHu
103 GeV
)and
Td ∼ 1 GeV
(1012 GeV
φ0
)(|µ|
103 GeV
)2
gives
nB
s∼ 10−10
(nL/nAD
10−2
)(1012 GeV
φ0
)3 (10−2 eV
mν
)(|µ|
103 GeV
)2 (10−1
αφ
)(mLHu
mφ(0)
)2
which suggestsφ0 ∼ 1012 GeV
![Page 53: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/53.jpg)
Dark matter candidates
Peccei-Quinn symmetry
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2HuHd + λχφχχ
DFSZ axion KSVZ axion
Axion
ma ∼Λ2
QCD
fawhere fa =
√2φ0
N
' 6.2× 10−6 eV
(1012 GeV
fa
)Axino
ma =1
16π2
∑χ
λ2χAχ
∼ 1 to 10 GeV
![Page 54: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/54.jpg)
Dark matter candidates
Peccei-Quinn symmetry
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2HuHd + λχφχχ
DFSZ axion
KSVZ axion
Axion
ma ∼Λ2
QCD
fawhere fa =
√2φ0
N
' 6.2× 10−6 eV
(1012 GeV
fa
)Axino
ma =1
16π2
∑χ
λ2χAχ
∼ 1 to 10 GeV
![Page 55: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/55.jpg)
Dark matter candidates
Peccei-Quinn symmetry
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2HuHd + λχφχχ
DFSZ axion KSVZ axion
Axion
ma ∼Λ2
QCD
fawhere fa =
√2φ0
N
' 6.2× 10−6 eV
(1012 GeV
fa
)Axino
ma =1
16π2
∑χ
λ2χAχ
∼ 1 to 10 GeV
![Page 56: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/56.jpg)
Dark matter candidates
Peccei-Quinn symmetry
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2HuHd + λχφχχ
DFSZ axion KSVZ axion
Axion
ma ∼Λ2
QCD
fawhere fa =
√2φ0
N
' 6.2× 10−6 eV
(1012 GeV
fa
)
Axino
ma =1
16π2
∑χ
λ2χAχ
∼ 1 to 10 GeV
![Page 57: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/57.jpg)
Dark matter candidates
Peccei-Quinn symmetry
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2HuHd + λχφχχ
DFSZ axion KSVZ axion
Axion
ma ∼Λ2
QCD
fawhere fa =
√2φ0
N
' 6.2× 10−6 eV
(1012 GeV
fa
)Axino
ma =1
16π2
∑χ
λ2χAχ
∼ 1 to 10 GeV
![Page 58: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/58.jpg)
Dark matter genesis
thermal inflation
flaton = saxinomatter domination
firstorder
phasetransition
radiationdomination
decay
axinos
decay
NLSP
decayaxions
QCD phase
transition
![Page 59: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/59.jpg)
Dark matter genesis
thermal inflation
flaton = saxinomatter domination
firstorder
phasetransition
radiationdomination
decay
axinos
decay
NLSP
decayaxions
QCD phase
transition
![Page 60: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/60.jpg)
Dark matter genesis
thermal inflation
flaton = saxinomatter domination
firstorder
phasetransition
radiationdomination
decay
axinos
decay
NLSP
decayaxions
QCD phase
transition
![Page 61: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/61.jpg)
Dark matter genesis
thermal inflation
flaton = saxinomatter domination
firstorder
phasetransition
radiationdomination
decay
axinos
decay
NLSP
decayaxions
QCD phase
transition
![Page 62: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/62.jpg)
Dark matter genesis
thermal inflation
flaton = saxinomatter domination
firstorder
phasetransition
radiationdomination
decay
axinos
decay
NLSP
decay
axionsQCD phase
transition
![Page 63: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/63.jpg)
Dark matter genesis
thermal inflation
flaton = saxinomatter domination
firstorder
phasetransition
radiationdomination
decay
axinos
decay
NLSP
decayaxions
QCD phase
transition
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Dark matter genesis
thermal inflation
flaton = saxinomatter domination
firstorder
phasetransition
radiationdomination
decay
axinos
decay
NLSP
decayaxions
QCD phase
transition
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Dark matter abundance
Flaton decays late
Td ∼ 1 GeV
(|µ|
103 GeV
)2 (1012 GeV
φ0
)
Axion
Misalignment
Ωa ∼ 3
(fa
1012 GeV
)1.2
×
1 for Td 1 GeV(
Td
1 GeV
)2
for Td 1 GeV
Axino
Flaton decay
Ωa ' 0.04( αa
10−1
)2 ( ma
1 GeV
)3(
1012 GeV
φ0
)2 (1 GeV
Td
)
Thermal NLSP decay
Ωa ∼ 10( ma
1 GeV
)(1012 GeV
φ0
)2
×
1 for Td
mN
7(7Td
mN
)7
for Td mN
7
![Page 66: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/66.jpg)
Dark matter abundance
Flaton decays late
Td ∼ 1 GeV
(|µ|
103 GeV
)2 (1012 GeV
φ0
)
Axion Misalignment
Ωa ∼ 3
(fa
1012 GeV
)1.2
×
1 for Td 1 GeV(
Td
1 GeV
)2
for Td 1 GeV
Axino
Flaton decay
Ωa ' 0.04( αa
10−1
)2 ( ma
1 GeV
)3(
1012 GeV
φ0
)2 (1 GeV
Td
)
Thermal NLSP decay
Ωa ∼ 10( ma
1 GeV
)(1012 GeV
φ0
)2
×
1 for Td
mN
7(7Td
mN
)7
for Td mN
7
![Page 67: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/67.jpg)
Dark matter abundance
Flaton decays late
Td ∼ 1 GeV
(|µ|
103 GeV
)2 (1012 GeV
φ0
)
Axion Misalignment
Ωa ∼ 3
(fa
1012 GeV
)1.2
×
1 for Td 1 GeV(
Td
1 GeV
)2
for Td 1 GeV
Axino Flaton decay
Ωa ' 0.04( αa
10−1
)2 ( ma
1 GeV
)3(
1012 GeV
φ0
)2 (1 GeV
Td
)
Thermal NLSP decay
Ωa ∼ 10( ma
1 GeV
)(1012 GeV
φ0
)2
×
1 for Td
mN
7(7Td
mN
)7
for Td mN
7
![Page 68: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/68.jpg)
Dark matter abundance
Flaton decays late
Td ∼ 1 GeV
(|µ|
103 GeV
)2 (1012 GeV
φ0
)
Axion Misalignment
Ωa ∼ 3
(fa
1012 GeV
)1.2
×
1 for Td 1 GeV(
Td
1 GeV
)2
for Td 1 GeV
Axino Flaton decay
Ωa ' 0.04( αa
10−1
)2 ( ma
1 GeV
)3(
1012 GeV
φ0
)2 (1 GeV
Td
)
Thermal NLSP decay
Ωa ∼ 10( ma
1 GeV
)(1012 GeV
φ0
)2
×
1 for Td
mN
7(7Td
mN
)7
for Td mN
7
![Page 69: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/69.jpg)
Dark matter abundanceFlaton decays late
Td ∼ 1 GeV
(|µ|
103 GeV
)2 (1012 GeV
φ0
)
Axion Misalignment
Ωa ∼ 3
(fa
1012 GeV
)1.2
×
1 for Td 1 GeV(
Td
1 GeV
)2
for Td 1 GeV
Axino Flaton decay
Ωa ' 0.04( αa
10−1
)2 ( ma
1 GeV
)3(
1012 GeV
φ0
)2 (1 GeV
Td
)
Thermal NLSP decay
Ωa ∼ 10( ma
1 GeV
)(1012 GeV
φ0
)2
×
1 for Td
mN
7(7Td
mN
)7
for Td mN
7
![Page 70: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/70.jpg)
Dark matter abundanceFlaton decays late
Td ∼ 1 GeV
(|µ|
103 GeV
)2 (1012 GeV
φ0
)
Axion Misalignment
Ωa ∼ 3
(fa
1012 GeV
)1.2
×
1 for Td 1 GeV(
Td
1 GeV
)2
for Td 1 GeV
Axino Flaton decay
Ωa ' 0.04( αa
10−1
)2 ( ma
1 GeV
)3(
1012 GeV
φ0
)2 (1 GeV
Td
)
Thermal NLSP decay
Ωa ∼ 10( ma
1 GeV
)(1012 GeV
φ0
)2
×
1 for Td
mN
7(7Td
mN
)7
for Td mN
7
![Page 71: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/71.jpg)
Dark matter abundanceFlaton decays late
Td ∼ 1 GeV
(|µ|
103 GeV
)2 (1012 GeV
φ0
)
Axion Misalignment
Ωa ∼ 3
(fa
1012 GeV
)1.2
×
1 for Td 1 GeV(
Td
1 GeV
)2
for Td 1 GeV
Axino Flaton decay
Ωa ' 0.04( αa
10−1
)2 ( ma
1 GeV
)3(
1012 GeV
φ0
)2 (1 GeV
Td
)
Thermal NLSP decay
Ωa ∼ 10( ma
1 GeV
)(1012 GeV
φ0
)2
×
1 for Td
mN
7(7Td
mN
)7
for Td mN
7
![Page 72: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/72.jpg)
Dark matter composition
|µ|GeV
Ω
102 103 10410−2
10−1
100
101
fa = 1012 GeVma = 1 GeV
axions
flatonaxinos
NLSPaxinos
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Axino LHC signal
NLSPs produced by the LHC decay to axinos plus Standard Model particles
LHCNLSP
axino
SM
with a decay length
1
ΓN→a∼
16πφ20
m3N
∼ 1 km
(200 GeV
mN
)3 ( φ0
1012 GeV
)2
and well constrained parameters
φ0 ∼ 1012 GeV
ma ' 1 GeV
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Axino LHC signal
NLSPs produced by the LHC decay to axinos plus Standard Model particles
LHCNLSP
axino
SM1 km
with a decay length
1
ΓN→a∼
16πφ20
m3N
∼ 1 km
(200 GeV
mN
)3 ( φ0
1012 GeV
)2
and well constrained parameters
φ0 ∼ 1012 GeV
ma ' 1 GeV
![Page 75: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/75.jpg)
Simple model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term drives m2φ < 0
thermal inflationbaryogenesis
axion
/axinodark matter
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Simple model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term drives m2φ < 0
thermal inflation
baryogenesis
axion
/axinodark matter
![Page 77: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/77.jpg)
Simple model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term drives m2φ < 0
thermal inflationbaryogenesisaxion
/axinodark matter
![Page 78: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/78.jpg)
Simple model
W = λuQHu u + λdQHd d + λeLHd e +1
2λν (LHu)2 + λµφ
2 HuHd + λχφχχ
MSSM neutrino masses MSSM µ-term drives m2φ < 0
thermal inflationbaryogenesisaxion/axinodark matter
![Page 79: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/79.jpg)
Rich cosmology
(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?
νR 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
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Rich cosmology
(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?
νR decay matter/antimatter?
moduli, gravitinos, . . . disaster
thermal inflation gravitational waves
φ decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
![Page 81: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/81.jpg)
Rich cosmology
(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?
νR decay matter/antimatter?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
φ decayQCD transition axion dark matter?
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
![Page 82: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/82.jpg)
Rich cosmology
(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?
νR decay matter/antimatter?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
φ decay axino dark matterQCD transition axion dark matter
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
![Page 83: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/83.jpg)
Rich cosmology
(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?
νR decay matter/antimatter?
moduli, gravitinos, . . . disaster
thermal inflation gravitational wavesLHu → 0 matter/antimatter
φ decay axino dark matterQCD transition axion dark matter
nucleosynthesis light elements
atom formation microwave backgroundgalaxy formation galaxies
vacuum energy dominates acceleration
![Page 84: A Minimal Supersymmetric Cosmological Model - …profstewart.org/papers/Beyond2010_Stewart.pdf · A Minimal Supersymmetric Cosmological Model Ewan Stewart ... 2 February 2010 Cape](https://reader031.vdocuments.us/reader031/viewer/2022022016/5b5e97927f8b9a8b4a8c949d/html5/thumbnails/84.jpg)
A Minimal Supersymmetric Cosmological Model
IntroductionStandard model of cosmologyModuli and gravitinos
A Minimal Supersymmetric Cosmological ModelMSSMMSCMThermal inflationBaryogenesisDark matter
SummarySimple modelRich cosmology