baryogenesis and dark matter
TRANSCRIPT
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@「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)
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@「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)
![Page 3: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/3.jpg)
@「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)
![Page 4: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/4.jpg)
@「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
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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
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Plan
Dark Matter in SUSY
Baryogenesis
Dark Matter and Baryogenesis in SUSY
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Dark Matter in SUSY
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Dark Matter in SUSYIn SUSY models + conserved R-parity, the Lightest SUSY Particle (= LSP) is stable.
➞ If neutral, Dark Matter candidate.
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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
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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
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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
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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!
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Baryogenesis
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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 )
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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
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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
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Baryon asymmetryin
BBN and CMB
Particle Data Group 2006
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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
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Baryon asymmetry is small ?!
Today.....
1
BaryonnB
s= 0.87 ! 10!10
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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......
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Baryon asymmetry is large ?!
Today.....
Baryon Anti-Baryon
nanti!baryon
s! 10!18nbaryon
s! 10!18
If there were no baryon asymmetry......
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Baryon asymmetry is large ?!
Today.....
Baryon Anti-Baryon
nanti!baryon
s! 10!18nbaryon
s! 10!18
If there were no baryon asymmetry......
! 10!10 !!
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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
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many baryogenesis scenarios...
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many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04
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many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04
(Too)
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many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04
(Too)
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many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04
(Too)
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many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04
(Too)
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many baryogenesis scenarios...talk by M.Shaposhnikov at DESY workshop’04
(Too)
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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。
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Thermal Leptogenesis by right-handed neutrino.
Affleck-Dine Baryogenesis (Q-ball, non-thermal DM)
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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.
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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
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Thermal Leptogenesis (答だけ)
nB
s=
neqNR1
s!
nL
nNR1
!nB
nL! !
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Thermal Leptogenesis (答だけ)0.35
nB
s=
neqNR1
s!
nL
nNR1
!nB
nL! !
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Thermal Leptogenesis (答だけ)0.004 0.35
nB
s=
neqNR1
s!
nL
nNR1
!nB
nL! !
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Thermal Leptogenesis (答だけ)0.004 0.35 <
! 0.18nB
s=
neqNR1
s!
nL
nNR1
!nB
nL! !
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Thermal Leptogenesis (答だけ)0.004 !1 0.35 <
! 0.18nB
s=
neqNR1
s!
nL
nNR1
!nB
nL! !
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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
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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.
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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
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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
"
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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
"
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gravitino problems
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gravitino problems
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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.
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gravitino problems
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stable (LSP) gravitino
gravitino problemsunstable gravitino
Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)
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stable (LSP) gravitino
gravitino problemsunstable gravitino
BBN
allowed
Fig. from Masahiro Ibe.(NOTE: precise line positions in this figure may be out-dated.)
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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.)
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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.)
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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.)
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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.)
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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.)
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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.)
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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.)
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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.)
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gravitino problems
Kohri, Moroi, Yotsuyanagi, ’05
unstable gravitino
4He
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gravitino problems
Kohri, Moroi, Yotsuyanagi, ’05
unstable gravitino
4He
thermalleptogenesis
m3/2 >! 10(?) TeV
(6 TeV?)
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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?
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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.)
![Page 69: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/69.jpg)
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。
![Page 70: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/70.jpg)
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
![Page 71: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/71.jpg)
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。
![Page 72: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/72.jpg)
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)
![Page 73: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/73.jpg)
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。
![Page 74: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/74.jpg)
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.)
![Page 75: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/75.jpg)
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?
![Page 76: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/76.jpg)
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
![Page 77: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/77.jpg)
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
![Page 78: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/78.jpg)
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
![Page 79: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/79.jpg)
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
![Page 80: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/80.jpg)
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
![Page 81: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/81.jpg)
まとめ(?) ・・・Dark Matter を見て Baryogenesis について何か言えるか?
![Page 82: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/82.jpg)
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。
![Page 83: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/83.jpg)
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。)
![Page 84: Baryogenesis and Dark Matter](https://reader034.vdocuments.site/reader034/viewer/2022051411/547faadeb37959932b8b5967/html5/thumbnails/84.jpg)
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。)