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Baryogenesis and Dark Matter
Transcript of 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。)