baryogenesis and dark matter

＠「宇宙初期における時空と物質の進化」

2007年5月、東京大学

Baryogenesis and Dark Matter

浜口幸一（東京大学）

＠「宇宙初期における時空と物質の進化」

2007年5月、東京大学

Baryogenesis and Dark Matter

浜口幸一（東京大学）

＠「宇宙初期における時空と物質の進化」

2007年5月、東京大学

Baryogenesis and Dark Matter

浜口幸一（東京大学）

＠「宇宙初期における時空と物質の進化」

2007年5月、東京大学

Baryogenesis and Dark Matter

浜口幸一（東京大学）

in SUSY

Gravitino Gravitino Interaction: extremely weak

suppressed by (or )

Gravitino Mass: model dependent

!1F

!1

MPm eG!

1MP

eV keV MeV GeV TeV

GMSBgMSB̃

AMSB, mMSB

gravity-MSB

Plan

Dark Matter in SUSY

Baryogenesis

Dark Matter and Baryogenesis in SUSY

Dark Matter in SUSY

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

➞ If neutral, Dark Matter candidate.

Dark Matter candidates in SUSY Standard Model

In SUSY Standard Model in SUGRA,.....

squarks :!

"uL

"dL

#

i

"uRi"dRi

sleptons :!

"!L

"eL

#

i"eRi

gauginos and higgssinos : ""0i , $"±

i , %ggravitino : %G

Dark Matter candidates in SUSY Standard Model

In SUSY Standard Model in SUGRA,.....

neutral and color-singlet

squarks :!

"uL

"dL

#

i

"uRi"dRi

sleptons :!

"!L

"eL

#

i"eRi

gauginos and higgssinos : ""0i , $"±

i , %ggravitino : %G

Dark Matter candidates in SUSY Standard Model

In SUSY Standard Model in SUGRA,.....

neutral and color-singlet

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

squarks :!

"uL

"dL

#

i

"uRi"dRi

sleptons :!

"!L

"eL

#

i"eRi

gauginos and higgssinos : ""0i , $"±

i , %ggravitino : %G

Dark Matter candidates in SUSY Standard Model

In SUSY Standard Model in SUGRA,.....

neutral and color-singlet

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

squarks :!

"uL

"dL

#

i

"uRi"dRi

sleptons :!

"!L

"eL

#

i"eRi

gauginos and higgssinos : ""0i , $"±

i , %ggravitino : %G

Only Neutralino and Gravitono are viable candidates!

Baryogenesis

Motivation観測されている宇宙のbaryon asymmetry

（物質・反物質の非対称性) を説明したい。

WMAP 3 years (2006)

nB

s= (0.87 ± 0.03) ! 10!10

バリオン数密度

エントロピー密度(～ 7×photon密度 )

inflation

thermal historytime temperature

～ 1 sec ～ 1 MeV Big Bang Nucleosynthesis=! D,4 He, · · ·

～ 1 eV matter-radiation equality

～ 0.3 eV Last Scattering Surface(photon becomes free)

～ 14 Gyr ～ 2.75 K CMBR observed

??? ???

??????nB

s! 0

inflation

thermal historytime temperature

～ 1 sec ～ 1 MeV Big Bang Nucleosynthesis=! D,4 He, · · ·

～ 1 eV matter-radiation equality

～ 0.3 eV Last Scattering Surface(photon becomes free)

～ 14 Gyr ～ 2.75 K CMBR observed

??? ??? Baryogenesis !nB

s" 10!10

??????nB

s! 0

Baryon asymmetryin

BBN and CMB

Particle Data Group 2006

At high temperature......

300,000,000 + 1 300,000,000

Baryon asymmetry is small ?!

Baryon

nbaryon

s! 0.03

Anti-Baryon

nanti!baryon

s! 0.03

Baryon asymmetry is small ?!

Today.....

1

BaryonnB

s= 0.87 ! 10!10

At high temperature......

300,000,000 300,000,000

Baryon asymmetry is large ?!

Baryon

nbaryon

s! 0.03

Anti-Baryon

nanti!baryon

s! 0.03

If there were no baryon asymmetry......

Baryon asymmetry is large ?!

Today.....

Baryon Anti-Baryon

nanti!baryon

s! 10!18nbaryon

s! 10!18

If there were no baryon asymmetry......

Baryon asymmetry is large ?!

Today.....

Baryon Anti-Baryon

nanti!baryon

s! 10!18nbaryon

s! 10!18

If there were no baryon asymmetry......

! 10!10 !!

Sakharov’s 3 conditions

(1) B

(2) C CPand

(3) Departure from equilibrium

!B > 0 process

!B < 0 processdifferent

rate

B = 0 B > 0

Sakharov ’67

many baryogenesis scenarios...

many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04

many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04

(Too)

many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04

(Too)

many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04

(Too)

many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04

(Too)

many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04

(Too)

Dark Matter and Baryogenesis in SUSY

まずはお気に入りの Baryogenesis を選ぶ。→ Dark Matterについて考える。→ テストする方法を考える。

Thermal Leptogenesis by right-handed neutrino.

Affleck-Dine Baryogenesis (Q-ball, non-thermal DM)

Thermal Leptogenesis by right-handed neutrino.

Affleck-Dine Baryogenesis (Q-ball, non-thermal DM)

☛ see the Next Talk by Nakayama-san.

• Simplest !! 標準模型に right-handed neutrino

を入れるだけ。• 何にもしないで熱浴に入れて放っておけば出来る。

☛ This talk.

Leptogenesis by decay: OverviewNR

?nB != 0

!nL = n! ! n!

"= 0

"

NR! + H

! + H!

decay

sphaleron

2

31depends onthe scenario

nB

s=

nNR

s!

nL

nNR

!nB

nL

1 2 3

Thermal Leptogenesis （答だけ）

nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

Thermal Leptogenesis （答だけ）0.35

nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

Thermal Leptogenesis （答だけ）0.004 0.35

nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

Thermal Leptogenesis （答だけ）0.004 0.35 <

! 0.18nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

Thermal Leptogenesis （答だけ）0.004 !1 0.35 <

! 0.18nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

Thermal Leptogenesis （答だけ）0.004 !1 0.35 <

! 0.18nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

KH, Murayama, Yanagida,’01neutrino mass!

!1 ! "3

16"

M1

#H$2Im

!h m!

! hT"11

(hh†)11

= "3

16"

M1

#H$2m!3 #e! #e! % 1

Thermal Leptogenesis （答だけ）0.004 !1 0.35 <

! 0.18nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

KH, Murayama, Yanagida,’01neutrino mass!

!1 ! "3

16"

M1

#H$2Im

!h m!

! hT"11

(hh†)11

= "3

16"

M1

#H$2m!3 #e! #e! % 1

!e! =Im

!(h̃13)2 + (h̃12)2 m!2

m!3+ (h̃11)2 m!1

m!3

"

|h̃13|2 + |h̃12|2 + |h̃11|2

where h̃ij = hi!U!!j (m")!# = U!iU#im"

diagi

KH, Dr.thesis,’02.

Thermal Leptogenesis （答だけ）0.004 !1 0.35 <

! 0.18nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

KH, Murayama, Yanagida,’01neutrino mass!

!1 ! "3

16"

M1

#H$2Im

!h m!

! hT"11

(hh†)11

= "3

16"

M1

#H$2m!3 #e! #e! % 1

0.004 !1 0.35 <! 0.18

Thermal Leptogenesis （答だけ）

nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

= 0.25 ! 10!10

!M1

109 GeV

" !m!3

0.05 eV

"!e!

!"

0.18

"

nB/s ! (0.87 ± 0.03) " 10!10To explain the observed baryon asymmetry,

M1 >! 3 " 109 GeV TR >

! 3 " 109 GeV

Davidson, Ibarra, ’02, Buchmuller, Di Bari, Plumacher, ’02

0.004 !1 0.35 <! 0.18

Thermal Leptogenesis （答だけ）

nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !

= 0.25 ! 10!10

!M1

109 GeV

" !m!3

0.05 eV

"!e!

!"

0.18

"

gravitino problems

gravitino problems

gravitino problems注意：インフラトンから直接作られる成分もかなり厳しい。

☛ see the Talk by Takahashi(F)-kun.

gravitino problems

stable (LSP) gravitino

gravitino problemsunstable gravitino

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

stable (LSP) gravitino

gravitino problemsunstable gravitino

BBN

allowed

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

stable (LSP) gravitino

gravitino problemsunstable gravitino

BBN

allowed

LSP from gravitino

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

stable (LSP) gravitino

gravitino problemsunstable gravitino

overclosure

allowed

BBN

allowed

LSP from gravitino

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

stable (LSP) gravitino

gravitino problemsunstable gravitino

overclosure

allowed

BBN

allowed

LSP from gravitino

16 eV

allo

wed

warm DM

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

gravitino problemsstable (LSP) gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

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

gravitino problemsstable (LSP) gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

gravitino problemsstable (LSP) gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

gravitino problemsstable (LSP) gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

gravitino problemsstable (LSP) gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

gravitino problems

Kohri, Moroi, Yotsuyanagi, ’05

unstable gravitino

4He

gravitino problems

Kohri, Moroi, Yotsuyanagi, ’05

unstable gravitino

4He

thermalleptogenesis

m3/2 >! 10(?) TeV

(6 TeV?)

gravitino problems

Kohri, Moroi, Yotsuyanagi, ’05

unstable gravitino

4He

thermalleptogenesis

m3/2 >! 10(?) TeV

(6 TeV?)

先生（川崎さん）質問！

この３つの線はどれが正しいのですか？

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

Dark Matter の観点からこの図を眺めてみる。

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

Dark Matter の観点からこの図を眺めてみる。

gravitino LSPでもCDMじゃない。→ DMはaxionか何か

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

Dark Matter の観点からこの図を眺めてみる。

gravitino LSPでもCDMじゃない。→ DMはaxionか何か

gravitino LSP→ gravitino DM。

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

Dark Matter の観点からこの図を眺めてみる。

gravitino LSPでもCDMじゃない。→ DMはaxionか何か

gravitino LSP→ gravitino DM。

(多分)Wino-like LSP→ Wino DM。(non-thermal)

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

Dark Matter の観点からこの図を眺めてみる。

gravitino LSPでもCDMじゃない。→ DMはaxionか何か

gravitino LSP→ gravitino DM。

(多分)Wino-like LSP→ Wino DM。(non-thermal)

例えば Standard(?)な thermal relic Bino-like DMだとthermal leptogenesis は苦しいかも。

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

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

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)テスト出来るか？

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)テスト出来るか？

gravitino massLHC/ILC で測れます。cf.) KH, Shirai, Yanagida ’07

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)テスト出来るか？

gravitino massLHC/ILC で測れます。cf.) KH, Shirai, Yanagida ’07

gravitino mass (頑張れば) 測れます。 cf.) Buchmuller, KH, Ratz, Yanagida ’04

KH, Kuno, Nakaya, Nojiri ’04KH, Nojiri, de Roeck ’07

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)テスト出来るか？

gravitino massLHC/ILC で測れます。cf.) KH, Shirai, Yanagida ’07

gravitino mass (頑張れば) 測れます。 cf.) Buchmuller, KH, Ratz, Yanagida ’04

KH, Kuno, Nakaya, Nojiri ’04KH, Nojiri, de Roeck ’07

Wino mass LHC+ILCで測れます。cf.) Asai, Moroi, Yanagida ’07

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)テスト出来るか？

gravitino massLHC/ILC で測れます。cf.) KH, Shirai, Yanagida ’07

gravitino mass (頑張れば) 測れます。 cf.) Buchmuller, KH, Ratz, Yanagida ’04

KH, Kuno, Nakaya, Nojiri ’04KH, Nojiri, de Roeck ’07

Wino mass LHC+ILCで測れます。cf.) Asai, Moroi, Yanagida ’07

特にここについては Planck scale が測れるかも (BHRY’04)

とか、実は Catalyzed BBN で厳しい (Pospelov’06; KH, Hatsuda, Kamimura, Kino, Yanagida’07; Kawasaki, Kohri, Moroi ’07 )とか、でもentropy productionがあれば大丈夫(Buchmuller, KH, Ibe, Yanagida’06) とか、R-parityが破れていてもgravitino DMがviableだ (Buchmuller, Covi, KH, Ibarra, Yanagida’06)

とか、いろいろ話したい事はありますが・・・またの機会

gravitino problemsstable gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis

Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)テスト出来るか？

gravitino massLHC/ILC で測れます。cf.) KH, Shirai, Yanagida ’07

gravitino mass (頑張れば) 測れます。 cf.) Buchmuller, KH, Ratz, Yanagida ’04

KH, Kuno, Nakaya, Nojiri ’04KH, Nojiri, de Roeck ’07

Wino mass LHC+ILCで測れます。cf.) Asai, Moroi, Yanagida ’07

まとめ(?) ・・・Dark Matter を見て Baryogenesis について何か言えるか？

まとめ(?) ・・・Dark Matter を見て Baryogenesis について何か言えるか？

LHC/ILCでBino-like LSP、計算したらthermal relic ばっちり（+出来れば detection) 　　→ thermal leptogenesis は苦しめ。

まとめ(?) ・・・Dark Matter を見て Baryogenesis について何か言えるか？

LHC/ILCでBino-like LSP、計算したらthermal relic ばっちり（+出来れば detection) 　　→ thermal leptogenesis は苦しめ。 LHC/ILCでWino-like LSP、計算したらthermal relicでは足りない（+ 出来ればdetection)→ non-thermal Wino DM→ thermal leptogenesis OK。 (Affleck-Dine + Q-ball の可能性も面白い。)

まとめ(?) ・・・Dark Matter を見て Baryogenesis について何か言えるか？

LHC/ILCでBino-like LSP、計算したらthermal relic ばっちり（+出来れば detection) 　　→ thermal leptogenesis は苦しめ。 LHC/ILCでWino-like LSP、計算したらthermal relicでは足りない（+ 出来ればdetection)→ non-thermal Wino DM→ thermal leptogenesis OK。 (Affleck-Dine + Q-ball の可能性も面白い。)

LHC/ILCでGravitino-LSP、mass測ったらconsistent,　→thermal leptogenesis OK。 (Affleck-Dine + Q-ball の可能性も面白い。)