at 中央大学理工学部, February ’09Koichi Hamaguchi (Tokyo U.)

グラビティーノLSPを持つ超対称標準模型とLHCでの検証可能性

Review+ works with W.Buchmüller, A.de Roeck, T.Hatsuda, M.Kamimura, Y.Kino, Y.Kuno, T.Nakaya, M.M.Nojiri, M.Ratz, T. T. Yanagida

Plan

Gravitino と SUSY models

Gravitino LSP と LHC での物理

Gravitino と Cosmology

Gravitino と SUSY models

Introduction

Introduction

• ... has been remarkably successful. But......

Introduction

Difficulties

Introduction

(1) naturalness problem

Difficulties

(fime tuning like 1.0000000000000000000000000000001 - 1)

Introduction

(1) naturalness problem

Difficulties

(2) towards unification

Introduction

(1) naturalness problem

Difficulties

(2) towards unification

electricity

magnetismelectro-

magnetism

“weak” force

electroweak

“strong” force

Standard Model

SU(2) x U(1)

SU(3)

Introduction

(1) naturalness problem

Difficulties

(2) towards unification

electricity

magnetismelectro-

magnetism

“weak” force

electroweak

“strong” force

Standard Model

SU(2) x U(1)

SU(3)

Grand Unified Theory

SU(5) ? SO(10) ?

?

Introduction

(1) naturalness problem

Difficulties

(2) towards unification

electricity

magnetismelectro-

magnetism

“weak” force

electroweak

“strong” force

Standard Model

SU(2) x U(1)

SU(3)

Grand Unified Theory

SU(5) ? SO(10) ?

?5 10 15

10

20

30

40

50

60

Log10!Q"GeV#

1"Α i

Grand Unified Theory predicts unification of three couplings at high energy.

high energy (short distance)

1 / c

oupl

ing

SU(3)

SU(2)

U(1)

experimental input

theoretical prediction

Introduction

(1) naturalness problem

Difficulties

(2) towards unification

electricity

magnetismelectro-

magnetism

“weak” force

electroweak

“strong” force

Standard Model

SU(2) x U(1)

SU(3)

Grand Unified Theory

SU(5) ? SO(10) ?

?5 10 15

10

20

30

40

50

60

Log10!Q"GeV#

1"Α i

Grand Unified Theory predicts unification of three couplings at high energy.

high energy (short distance)

1 / c

oupl

ing

SU(3)

SU(2)

U(1)

experimental input

theoretical prediction

But,.....

Introduction

(1) naturalness problem

Difficulties

(2) towards unification(3) no dark matter candidate

Introduction

(1) naturalness problem

Difficulties

(2) towards unification(3) no dark matter candidate

None of them can explain the observed dark matter

Introduction

Difficulties

(1) naturalness problem(2) towards unification(3) no dark matter candidate

Introduction

Difficulties

(1) naturalness problem(2) towards unification(3) no dark matter candidate Somethin

g beyond the Stan

dard Model is nece

ssary!!

Introductionbeyond the Standard Model

Supersymmetry?

Extra dimensions? (flat or warped?)

???

Introductionbeyond the Standard Model

Supersymmetry Extra dimensions? (flat or warped?)

???

Supersymmetry (SUSY)

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

(1) solves the naturalness problem

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

(1) solves the naturalness problem(2) leads to coupling unification

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

(1) solves the naturalness problem

high energy (short distance)

1 / c

oupl

ing

SU(3)

SU(2)

U(1)

experimental input

5 10 1510

20

30

40

50

60

Log10!Q"GeV#

1"Α i

(2) leads to coupling unification

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

(1) solves the naturalness problem

high energy (short distance)

1 / c

oupl

ing

SU(3)

SU(2)

U(1)

experimental input

theoretical prediction (SUSY)

5 10 1510

20

30

40

50

60

Log10!Q"GeV#

1"Α i beautiful unification!!

(2) leads to coupling unification

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

(1) solves the naturalness problem(2) leads to coupling unification(3) has dark matter candidate

Dark Matter in SUSYR-parity ... to avoid too rapid baryon/lepton number violationStandard Model particle: A ➜ A SUSY partner particle: B ➜ -B

• B A₁ A₂ ........ forbidden B ➜ A₁ + A₂- + +

• B₁ B₂ A ....... allowed B₁ ➜ B₂ + A- - +

Interactions

Dark Matter in SUSYIn SUSY models + R-parity, the Lightest SUSY Particle (= LSP) is stable.

➞ If neutral, Dark Matter candidate!

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

(1) solves the naturalness problem(2) leads to coupling unification(3) has dark matter candidate

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

(1) solves the naturalness problem(2) leads to coupling unification(3) has dark matter candidate

Not d

iscove

red (y

et)

..... the leading candidate for the physics beyond the Standard ModelSupersymmetry

Not d

iscove

red (y

et)

We expect SUSY particles have O(0.1 - 1 TeV) masses.➔ will be discovered at the LHC (2009-)!!➔ new paradigm!!

1

Superstring∪

1

Superstring∪

1

Electroweak Symmetry と比べてみる

Electroweak Symmetry と比べてみる

Electroweak Symmetry と比べてみる

mV = g 〈ϕ〉gauge coupling

SUGRA coupling

gauge boson mass gravitino mass

Higgs VEV SUSY breaking VEV

m eG =1

√3MP

〈F 〉

GravitinoGravitino Interaction: extremely weak

suppressed by (or )

Gravitino Mass : model dependent

∼1F

∼1

MPm eG∼

1MP

100TeV 106 GeV

GMSBgMSB̃

AMSB, mMSB

gravity-MSB (mSUGRA 含む)

Gravitino が LSP になるモデル

m eG =1

√3MP

〈F 〉

eV keV MeV GeV TeV

107 GeV 108 GeV 109 GeV 1010 GeV 1011 GeV√〈F 〉

m eG

NLSP (Next-to-Lightest SUSY Particle)In Gravitino LSP scenario, the NLSP decay always include the gravitino.

∼1F

∼1

MPm eG

Interaction

NLSP (Next-to-Lightest SUSY Particle)In Gravitino LSP scenario, the NLSP decay always include the gravitino.

Γ(τ̃ → G̃τ ) "m5τ̃

48πm2G̃

M2pl

(1 −

m2G̃

m2τ̃

)4For a slepton NLSP,.....

eV keV MeV GeVe.g., for mτ̃ = 100 GeV ,

mG̃

ττ̃μs secmsnsps

kmmmmcττ̃

day

Lifetime (decay length) of NLSP stau

Gravitino LSP と LHC での物理と NLSP

•Why Gravitino LSP ?

•Why Gravitino LSP ?

squarks :(

ũLd̃L

)

i

ũRid̃Ri

sleptons :(

ν̃LẽL

)

iẽRi

gauginos and higgssinos : χ̃0i , χ̃±i , g̃

gravitino : G̃

• ..... among 29 SUSY particles?

Dark Matter candidates in SUSY Standard Model

squarks :(

ũLd̃L

)

i

ũRid̃Ri

sleptons :(

ν̃LẽL

)

iẽRi

gauginos and higgssinos : χ̃0i , χ̃±i , g̃

gravitino : G̃

•Why Gravitino LSP ?

Dark Matter candidates in SUSY Standard Model

neutral and color-singlet

squarks :(

ũLd̃L

)

i

ũRid̃Ri

sleptons :(

ν̃LẽL

)

iẽRi

gauginos and higgssinos : χ̃0i , χ̃±i , g̃

gravitino : G̃

•Why Gravitino LSP ?

Dark Matter candidates in SUSY Standard Model

neutral and color-singlet

excluded by direct detection experiments(cf. Falk, Olive, Srednicki,’94)

squarks :(

ũLd̃L

)

i

ũRid̃Ri

sleptons :(

ν̃LẽL

)

iẽRi

gauginos and higgssinos : χ̃0i , χ̃±i , g̃

gravitino : G̃

•Why Gravitino LSP ?

Dark Matter candidates in SUSY Standard Model

neutral and color-singlet

excluded by direct detection experiments(cf. Falk, Olive, Srednicki,’94)

Only Neutralino and Gravitino are viable candidates!

squarks :(

ũLd̃L

)

i

ũRid̃Ri

sleptons :(

ν̃LẽL

)

iẽRi

gauginos and higgssinos : χ̃0i , χ̃±i , g̃

gravitino : G̃

•Why Gravitino LSP ?

neutralino LSP

SUSY models

•Why Gravitino LSP ?

gravitino LSP

others fifty-fifty?

•What is the NLSP ?

squarks :(

ũLd̃L

)

i

ũRid̃Ri

sleptons :(

ν̃LẽL

)

iẽRi

gauginos and higgssinos : χ̃0i , χ̃±i , g̃

gravitino : G̃

• ..... among 28 NLSP candidates?

!̃

•What is the NLSP ?• In general, from RGE, tendency is

• M(color singlet) < M(colored)

typical RG evolution (from S.P.Martin, hep-ph/9709356)

sleptons

squarksq̃

gluino

gauginoHiggsino

!̃

•What is the NLSP ?• In general, from RGE, tendency is

• M(color singlet) < M(colored)

typical RG evolution (from S.P.Martin, hep-ph/9709356)

• M(weak singlet) < M(weak charged)

sleptons

squarksq̃

(ν̃L"̃L

)!̃R

gluino

gauginoHiggsino

!̃

•What is the NLSP ?• In general, from RGE, tendency is

• M(color singlet) < M(colored)

typical RG evolution (from S.P.Martin, hep-ph/9709356)

• M(weak singlet) < M(weak charged) • M(3rd family) < M(1st and 2nd family)

sleptons

squarksq̃

(ν̃L"̃L

)!̃R

τ̃1ẽR, µ̃R

gluino

gauginoHiggsino

!̃

•What is the NLSP ?• In general, from RGE, tendency is

• M(color singlet) < M(colored)

typical RG evolution (from S.P.Martin, hep-ph/9709356)

• M(weak singlet) < M(weak charged) • M(3rd family) < M(1st and 2nd family)

sleptons

squarksq̃

(ν̃L"̃L

)!̃R

τ̃1ẽR, µ̃R

gluino

gauginoHiggsino

• In most cases, either Stau or Neutralino is the NLSP

•What is the NLSP ?

SUSY models

gravitino LSP

neutralinoLSP

Stau NLSP

Neutralino NLSP

others

eV keV MeV GeVe.g., for mτ̃ = 100 GeV ,

mG̃

ττ̃μs secmsnsps

kmmmmcττ̃

day

Γ(τ̃ → G̃τ ) "m5τ̃

48πm2G̃

M2pl

(1 −

m2G̃

m2τ̃

)4

NLSP lifetime

Lifetime (decay length) of NLSP stau

eV keV MeV GeVe.g., for mτ̃ = 100 GeV ,

mG̃

ττ̃μs secmsnsps

kmmmmcττ̃

day

Γ(τ̃ → G̃τ ) "m5τ̃

48πm2G̃

M2pl

(1 −

m2G̃

m2τ̃

)4

NLSP lifetime

Lifetime (decay length) of NLSP stau

Detector Size No In-flight decay,

but maybe accessible.

prompt decay

eV keV MeV GeVe.g., for mτ̃ = 100 GeV ,

mG̃

ττ̃μs secmsnsps

kmmmmcττ̃

day

Γ(τ̃ → G̃τ ) "m5τ̃

48πm2G̃

M2pl

(1 −

m2G̃

m2τ̃

)4

NLSP lifetime

Lifetime (decay length) of NLSP stau

Detector Size No In-flight decay,

but maybe accessible.

prompt decay

NLSPの寿命を測る事が重要なターゲット

=
SUSY
breaking
scale


























を測る事

(=
gravitino
mass








を測る事)

F =√

3 m eGMP

m eG

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる

寿命測れる

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる

寿命測れる

Kawagoe, Kobayashi, Nojiri, Ochi, ’03

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる

寿命測れる

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる？! 寿命測れる

寿命測れる

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる？! 寿命測れる

寿命測れる

時間があれば後ほど・・・

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる？! 寿命測れる寿命測れる？

寿命測れる

時間があれば後ほど・・・

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる？! 寿命測れる寿命測れる？

+ SUGRA test?!

寿命測れる

時間があれば後ほど・・・

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃0

寿命測れる？! 寿命測れる寿命測れる？

+ SUGRA test?!

寿命測れる

時間があれば後ほど・・・

We will see long-lived charged particle (like muon).τ̃τ̃

Spectacular events! Many SUSY informations can be obtained!

Fig. from CMS webpage Fig. from ATLAS webpage

But,..... we cannot see the stau decay (and gravitino)

Long-lived staus @ LHC

➔ We need to stop the sleptons.

Long-lived sleptons @ LHC

We would like to see the decay of slepton (into gravitino).

➔ We need to stop the sleptons.

Long-lived sleptons @ LHC

We would like to see the decay of slepton (into gravitino).

➔ We need to stop the sleptons.

Long-lived sleptons @ LHC

We would like to see the decay of slepton (into gravitino).

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810

12-10-8-6-4-20246810

-8-6-4-202468

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3.5m

15m

15m

CMS stopper-detector 5g/cm3

(total weight 8kt)

stopper-detectorMaybe... stoppers next to main detectors.

Hamaguchi, Nojiri, De Roeck’06

3.5m15m

➔ maybe possible to install stopper-detectors.

test of SUGRA

プランクスケールが LHC で測れる ?!

Planck scale measurementW.Buchmüller, K.Hamaguchi, M.Ratz, T.Yanagida ’04

Planck scale measurementW.Buchmüller, K.Hamaguchi, M.Ratz, T.Yanagida ’04

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3.5m

15m

15m

CMS stopper-detector 5g/cm3

(total weight 8kt)

stopper-detectorWe assume two stoppers next to CMS.

Hamaguchi, Nojiri, De Roeck’06

3.5m15m

➔ maybe possible to install stopper-detectors.

-12-10-8-6 -4-2 0 2 46

810

12-10-8-6-4-20246810

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3.5m

15m

15m

CMS stopper-detector 5g/cm3

(total weight 8kt)

stopper-detectorWe assume two stoppers next to CMS.

Hamaguchi, Nojiri, De Roeck’06

3.5m15m

➔ maybe possible to install stopper-detectors.

-6

-4

-2

0

2

4

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y-p

ositio

n[m

]

z-positon[m]

-6

-4

-2

0

2

4

6

10 12

x[m]

10.0

12.0

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x[m

]

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810

3.5m

15m

15m

CMS stopper-detector 5g/cm3

(total weight 8kt)

stopper-detectorWe assume two stoppers next to CMS.

Hamaguchi, Nojiri, De Roeck’06

3.5m15m

➔ maybe possible to install stopper-detectors.

-6

-4

-2

0

2

4

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y-p

ositio

n[m

]

z-positon[m]

-6

-4

-2

0

2

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10 12

x[m]

10.0

12.0

-6 -4 -2 0 2 4 6

x[m

]

0

20

40

60

80

100

120

140

160

0 20 40 60 80 100 120

(a)

Low Stat.Best Fit

Ejet [GeV]

num

ber

ofev

ents

/bi

n

0

2

4

6

8

10

50 55 60 65 70 75 80 85 90 95 100

(b)

Eτ [GeV]

2∆ln

L-1

-0.5

0

0.5

1

50 55 60 65 70 75 80 85 90 95 100

(c)

Eτ [GeV]P

τ

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3.5m

15m

15m

CMS stopper-detector 5g/cm3

(total weight 8kt)

stopper-detectorWe assume two stoppers next to CMS.

Hamaguchi, Nojiri, De Roeck’06

3.5m15m

➔ maybe possible to install stopper-detectors.

-6

-4

-2

0

2

4

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y-p

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n[m

]

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x[m]

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x[m

]

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(a)

Low Stat.Best Fit

Ejet [GeV]

num

ber

ofev

ents

/bi

n

0

2

4

6

8

10

50 55 60 65 70 75 80 85 90 95 100

(b)

Eτ [GeV]

2∆ln

L-1

-0.5

0

0.5

1

50 55 60 65 70 75 80 85 90 95 100

(c)

Eτ [GeV]P

τ

• What? Additional 8 kton detectors?! How expensive is it?!

• (Theorists are always bringing crazy ideas...)

an experi-mentalist

• What? Additional 8 kton detectors?! How expensive is it?!

• (Theorists are always bringing crazy ideas...)

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15m

15m

CMS stopper-detector 5g/cm3(total weight 8kt)

3.5m15m

an experi-mentalist

• What? Additional 8 kton detectors?! How expensive is it?!

• (Theorists are always bringing crazy ideas...)

-12-10-8-6 -4-2 0 2 46

810

12-10-8-6-4-20246810

-8-6-4-202468

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810

3.5m

15m

15m

CMS stopper-detector 5g/cm3(total weight 8kt)

3.5m15m

an experi-mentalist

(Theorists are always bringing crazy ideas.....)

What?!8kton additional detectors?!

You know how expensive it is?!!

• What? Additional 8 kton detectors?! How expensive is it?!

• (Theorists are always bringing crazy ideas...)

-12-10-8-6 -4-2 0 2 46

810

12-10-8-6-4-20246810

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810

3.5m

15m

15m

CMS stopper-detector 5g/cm3(total weight 8kt)

3.5m15m

an experi-mentalist

(Theorists are always bringing crazy ideas.....)

What?!8kton additional detectors?!

You know how expensive it is?!!

(... any better idea?) [work in progress...]

またの機会に・・・

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃

0

F determination F determination

F determination

+ SUGRA test?!

F determination

またの機会に・・・

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃

0

F determination F determination

F determination

+ SUGRA test?!

F determination

Let’s see

what the

LHC will

find..... !

Gravitino と Cosmology

どこかでDM生成

１秒より前のシナリオは色々工夫出来る

１秒より後は余計な事しちゃダメ

どこかでDM生成

Gravitino Problems

Sorry, I drop references.

(gravitinoがLSPの場合)

stable (LSP) gravitino unstable gravitino

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

stable (LSP) gravitino unstable gravitino

BBN

allowed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

stable (LSP) gravitino unstable gravitino

BBN

allowed

LSP from gravitino

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

stable (LSP) gravitino unstable gravitino

overclosure

allowed

BBN

allowed

LSP from gravitino

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

stable (LSP) gravitino unstable gravitino

overclosure

allowed

BBN

allowed

LSP from gravitino

16 eV

allo

wed

warm DM

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

stable (LSP) gravitino unstable gravitino

overclosure

allowed

BBN

allowed

LSP from gravitino

16 eV

allo

wed

warm DM

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

NLSP BBN

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

thermalleptogenesis

ここホントは6TeVくらい

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

thermalleptogenesis

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

thermalleptogenesis

nonthermalleptogenesis

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

thermalleptogenesis

nonthermalleptogenesis

Affleck Dinebaryogenesis

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

thermalleptogenesis

nonthermalleptogenesis

Affleck Dinebaryogenesis

In addition, direct production of gravitinos from inflaton ➜ exclude many inflation models

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

thermalleptogenesis

nonthermalleptogenesis

Affleck Dinebaryogenesis

In addition, direct production of gravitinos from inflaton ➜ exclude many inflation models

Fig. from Endo, Takahashi, Yanagida, ’07

stable (LSP) gravitino unstable gravitino

allowed

allowed16 eV

allo

wed

(NOTE: precise line positions in this figure may be out-dated.)

Gravitino Problems

Sorry, I drop references.

m eG / GeV

thermalleptogenesis

nonthermalleptogenesis

Affleck Dinebaryogenesis

In addition, direct production of gravitinos from inflaton ➜ exclude many inflation models

Fig. from Endo, Takahashi, Yanagida, ’07

実は、gravity-MSB
(mSUGRA含む）は

宇宙論的には非常に苦しい！

gravitino
と
cosmology


•実は、long-lived
particle
のヒントが既に見えているかもしれない・・・。

Fig. from Review of Particle Physics

Fig. from Review of Particle Physics

If there is a long-lived charged particle.... → affects the BBN!!1. decay’s effect 2. catalysis effect

Fig. from Review of Particle Physics

If there is a long-lived charged particle.... → affect the BBN!!1. decay’s effect 2. catalysis effect ☚

If there were negatively charged particle, X- at BBN,...

➔ bound states with positively charged nuclei.➔ new catalyzed reactions occur!

Catalyzed BBN (CBBN) Pospelov ’06

If there were negatively charged particle, X- at BBN,...

➔ bound states with positively charged nuclei.➔ new catalyzed reactions occur!

(1) strong constraints on X lifetime and abundance.

Pospelov ’06;.......; KH, Hatsuda, Kamimura, Kino, Yanagida ’07

catalyzed BBNstandard BBN

O(109) enhancement !!! ➔ too much Li6 !!!

Catalyzed BBN (CBBN) Pospelov ’06

If there were negatively charged particle, X- at BBN,...

➔ bound states with positively charged nuclei.➔ new catalyzed reactions occur!

Catalyzed BBN (CBBN) Pospelov ’06

(1) strong constraints on X lifetime and abundance.

(2) there may already exist a hint of this CBBN. ➔ Li7 problem.

Fig. from Review of Particle Physics

Fig. from Review of Particle Physics

“Li-7 problem”

Fig. from Review of Particle Physics

“Li-7 problem”

recently, reanalyzed byCyburt, Fields, Olive, 0808.2818

Fig. from Review of Particle Physics

“Li-7 problem”

recently, reanalyzed byCyburt, Fields, Olive, 0808.2818

“The Li problem remains and indeed exacerbated;

the discrepancy is now 4.2σ - 5.3σ.”

If there were negatively charged particle, X- at BBN,...

➔ bound states with positively charged nuclei.➔ new catalyzed reactions occur!

Catalyzed BBN (CBBN) Pospelov ’06

(1) strong constraints on X lifetime and abundance.

(2) there may already exist a hint of this CBBN. ➔ Li7 problem.

If there were negatively charged particle, X- at BBN,...

➔ bound states with positively charged nuclei.➔ new catalyzed reactions occur!

Catalyzed BBN (CBBN) Pospelov ’06

(1) strong constraints on X lifetime and abundance.

(2) there may already exist a hint of this CBBN. ➔ Li7 problem.

CBBN can solve it! (7Be X-)+p → (8B X-)+ΥPospelov,’06;+ Bird, Koopmans, Pospelov,’07+ Kusakabe, Kajino, Boyd, Yoshida, Mathews,’07,+ Kamimura, Kino, Hiyama,’08,+ Jittoh, Kohri, Koike, Sato, Shimomura, Yamanaka,’07,’08

If there were negatively charged particle, X- at BBN,...

➔ bound states with positively charged nuclei.➔ new catalyzed reactions occur!

Catalyzed BBN (CBBN) Pospelov ’06

(1) strong constraints on X lifetime and abundance.

(2) there may already exist a hint of this CBBN. ➔ Li7 problem.

CBBN can solve it! (7Be X-)+p → (8B X-)+ΥPospelov,’06;+ Bird, Koopmans, Pospelov,’07+ Kusakabe, Kajino, Boyd, Yoshida, Mathews,’07,+ Kamimura, Kino, Hiyama,’08,+ Jittoh, Kohri, Koike, Sato, Shimomura, Yamanaka,’07,’08

..... ifX lifetime is O(1000) sec.

If there were negatively charged particle, X- at BBN,...

➔ bound states with positively charged nuclei.➔ new catalyzed reactions occur!

Catalyzed BBN (CBBN) Pospelov ’06

(1) strong constraints on X lifetime and abundance.

(2) there may already exist a hint of this CBBN. ➔ Li7 problem.

CBBN can solve it! (7Be X-)+p → (8B X-)+ΥPospelov,’06;+ Bird, Koopmans, Pospelov,’07+ Kusakabe, Kajino, Boyd, Yoshida, Mathews,’07,+ Kamimura, Kino, Hiyama,’08,+ Jittoh, Kohri, Koike, Sato, Shimomura, Yamanaka,’07,’08

..... ifX lifetime is O(1000) sec.

☛ Such a long-live

d charged particle

naturally arises in

SUSY models with

gravitino LSP + sta

u NLSP!!

またの機会に・・・

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃

0

F determination F determination

F determination

+ SUGRA test?!

F determination

Gravitino LSP at LHC: Summary

またの機会に・・・

Gravitino and

NLSP at the LHC

G̃ G̃

NLSP

G̃

NLSP

τ̃ NLSP“kink” in

charged trackcharged track

χ̃0 NLSP 2γ + ET,missnon-pointing

photon the same asLSP signal....χ̃

0

F determination F determination

F determination

+ SUGRA test?!

F determination

Let’s see

what the

LHC will

find..... !

Gravitino LSP at LHC: Summary