Strong SO(10)-inspired leptogenesis predictions and justification - - PowerPoint PPT Presentation
Luca Marzola Strong SO(10)-inspired leptogenesis predictions and justification Reference papers: E. Bertuzzo, P . Di Bari, L.M. - Nucl.Phys.B849:521-548,2011 P . Di Bari, L. M. - in preparation Rencontres de Moriond, E.W.
– predictions and justification –
Rencontres de Moriond, E.W. session, 3-10/03/2012
Luca Marzola Reference papers:
. Di Bari, L.M. - Nucl.Phys.B849:521-548,2011
. Di Bari, L. M. - in preparation
18 new parameters: hαi, Mi.
L = LSM + iNRi@µµNRi − hαi`LαNRi ˜ Φ − 1 2
3
X
i=1
Nc
RiDMiNRi + H.c.
Dx:=diag(X1, X2,X3)
18 new parameters: hαi, Mi.
L = LSM + iNRi@µµNRi − hαi`LαNRi ˜ Φ − 1 2
3
X
i=1
Nc
RiDMiNRi + H.c.
mν = −mD 1 DM mT
D
mD = vh
−Dm = U †mνU ∗
mD = V †
LDmDUR
Dx:=diag(X1, X2,X3) assuming diagonalised charged leptons
18 new parameters: hαi, Mi.
L = LSM + iNRi@µµNRi − hαi`LαNRi ˜ Φ − 1 2
3
X
i=1
Nc
RiDMiNRi + H.c.
mν = −mD 1 DM mT
D
mD = vh
−Dm = U †mνU ∗
mD = V †
LDmDUR
P . Di Bari, A. Riotto; 2008
M−1 := D−1
mDVLUDmU T V T L D−1 mD ≡ URD−1 M U T R
given by diagonalisation of M−1(M−1)†
Dx:=diag(X1, X2,X3) assuming diagonalised charged leptons
18 new parameters: hαi, Mi.
L = LSM + iNRi@µµNRi − hαi`LαNRi ˜ Φ − 1 2
3
X
i=1
Nc
RiDMiNRi + H.c.
mν = −mD 1 DM mT
D
mD = vh
−Dm = U †mνU ∗
mD = V †
LDmDUR
P . Di Bari, A. Riotto; 2008
M−1 := D−1
mDVLUDmU T V T L D−1 mD ≡ URD−1 M U T R
given by diagonalisation of M−1(M−1)† 15 + 3 → 6 + 3 + 6 + 3
Dx:=diag(X1, X2,X3) assuming diagonalised charged leptons
18 new parameters: hαi, Mi.
L = LSM + iNRi@µµNRi − hαi`LαNRi ˜ Φ − 1 2
3
X
i=1
Nc
RiDMiNRi + H.c.
mν = −mD 1 DM mT
D
mD = vh
−Dm = U †mνU ∗
mD = V †
LDmDUR
P . Di Bari, A. Riotto; 2008
M−1 := D−1
mDVLUDmU T V T L D−1 mD ≡ URD−1 M U T R
given by diagonalisation of M−1(M−1)† 15 + 3 → 6 + 3 + 6 + 3
neutrino oscillation experiments SO(10)-inspired conditions
Dx:=diag(X1, X2,X3) assuming diagonalised charged leptons
mDi parametrized by αi ~ O(1)...but only α2 matters!
DmD = α1mu α2mc α3mt
mDi parametrized by αi ~ O(1)...but only α2 matters!
DmD = α1mu α2mc α3mt
Strongly hierarchical RH neutrino mass spectrum:
M3 > 1012 GeV > M2 > 109 GeV M1
mDi parametrized by αi ~ O(1)...but only α2 matters!
DmD = α1mu α2mc α3mt
Strongly hierarchical RH neutrino mass spectrum:
M3 > 1012 GeV > M2 > 109 GeV M1
P . Di Bari, A. Riotto; 2010
Nlep,f
B−L ' P 0 2e
P 0
˜ τ2
ε˜
τ2κ(K2, K˜ τ2)e− 3π
8 K1e + P 0
2µ
P 0
˜ τ2
ε˜
τ2κ(K2, K˜ τ2)e− 3π
8 K1µ + ε2τκ(K2, K2τ)e− 3π 8 K1τ
ηCMB
B
∼ 10−9
ηlep
B ∼ 10−2N lep,f B−L
Npreex,0
B−L
∼ O(1)
ηB ' 10−2 ⇣ Nlep,f
B−L + Npreex,f B−L
⌘ 10−9
ηCMB
B
∼ 10−9
ηlep
B ∼ 10−2N lep,f B−L
Npreex,0
B−L
∼ O(1)
ηB ' 10−2 ⇣ Nlep,f
B−L + Npreex,f B−L
⌘ 10−9
Universe after inflation era)
Npreex,0
B−L
ηCMB
B
∼ 10−9
Vanilla Leptogenesis
parameter space, respected ONLY by the
휏-N2 dominated scenario
ηCMB
B
∼ 10−9
ηlep
B ∼ 10−2N lep,f B−L
Npreex,0
B−L
∼ O(1)
ηB ' 10−2 ⇣ Nlep,f
B−L + Npreex,f B−L
⌘ 10−9
Universe after inflation era)
Npreex,0
B−L
ηB ' 10−2 ⇣ N lep,f
B−L + N preex,f B−L
⌘ ' 10−9
. Di Bari, L.M.; 2011
Vanilla Leptogenesis
parameter space, respected ONLY by the
휏-N2 dominated scenario
N2 dominated leptogenesis + strong washout: K2>>1 Asymmetric washout from N1: K1e, K1µ>>1; K1휏~1
ηCMB
B
∼ 10−9
ηlep
B ∼ 10−2N lep,f B−L
Npreex,0
B−L
∼ O(1)
ηB ' 10−2 ⇣ Nlep,f
B−L + Npreex,f B−L
⌘ 10−9
Universe after inflation era)
Npreex,0
B−L
ηB ' 10−2 ⇣ N lep,f
B−L + N preex,f B−L
⌘ ' 10−9
. Di Bari, L.M.; 2011
휃13 vs m1 휃23 vs m1 mee vs m1 α2 =5, 1⩽VL⩽CKM, normal ordering. =0, 10-3, 10-2, 10-1 ⍴ vs σ (1/π) JCP vs 휃13 Mi vs m1
P . Di Bari, L.M. - Work in progress
N preex,0
B−L
experimental results
conditions
the model