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）

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



neutral and color-singlet

squarks :!

"uL

"dL

#

i

"uRi"dRi

sleptons :!

"!L

"eL

#

i"eRi






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

squarks :!

"uL

"dL

#

i

"uRi"dRi

sleptons :!

"!L

"eL

#

i"eRi






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

squarks :!

"uL

"dL

#

i

"uRi"dRi

sleptons :!

"!L

"eL

#

i"eRi



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......


Today.....

Baryon Anti-Baryon

nanti!baryon

s! 10!18nbaryon

s! 10!18



Today.....

Baryon Anti-Baryon

nanti!baryon

s! 10!18nbaryon

s! 10!18


! 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)

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! !


! 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


! 0.18nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !


!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.


! 0.18nB

s=

neqNR1

s!

nL

nNR1

!nB

nL! !


!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


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


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.)



BBN

allowed




BBN

allowed

LSP from gravitino




overclosure

allowed

BBN

allowed

LSP from gravitino




overclosure

allowed

BBN

allowed

LSP from gravitino

16 eV

allo

wed

warm DM


gravitino problemsstable (LSP) gravitino unstable gravitino

allowedallowed

16 eV

allo

wed


gravitino problemsstable (LSP) gravitino unstable gravitino

allowedallowed

16 eV

allo

wed

thermalleptogenesis


gravitino problems

Kohri, Moroi, Yotsuyanagi, ’05

unstable gravitino

4He

gravitino problems


unstable gravitino

4He

thermalleptogenesis

m3/2 >! 10(?) TeV

(6 TeV?)

gravitino problems


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



allowedallowed

16 eV

allo

wed

thermalleptogenesis


Dark Matter の観点からこの図を眺めてみる。


allowedallowed

16 eV

allo

wed

thermalleptogenesis



gravitino LSPでもCDMじゃない。→ DMはaxionか何か


allowedallowed

16 eV

allo

wed

thermalleptogenesis




gravitino LSP→ gravitino DM。


allowedallowed

16 eV

allo

wed

thermalleptogenesis





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


allowedallowed

16 eV

allo

wed

thermalleptogenesis





(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。


allowedallowed

16 eV

allo

wed

thermalleptogenesis



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？


allowedallowed

16 eV

allo

wed

thermalleptogenesis


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


allowedallowed

16 eV

allo

wed

thermalleptogenesis



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


allowedallowed

16 eV

allo

wed

thermalleptogenesis





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


allowedallowed

16 eV

allo

wed

thermalleptogenesis






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


allowedallowed

16 eV

allo

wed

thermalleptogenesis






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。)

baryogenesis and dark matter

Documents