Physics beyond the Standard Model: Neutrinos & Dark matter
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1 Physics beyond the Standard Model: Neutrinos & Dark matter José W F Valle PASCOS 2013, Taiwan 1
2 Where do neutrinos come from? 336 / cm3: bilions of Cosmic neutrinos Cross us every second confirmation Necessary to revise Standard model
3 LEPTON MIXING MATRIX Schechter & JV PRD22 (1980) 2227 & PDG Rodejohann, JV Phys.Rev. D84 (2011) Presence of majorana phases (cf KM) Do not affect (standard) oscillations but Crucial to describe L-violating processes K Rectangular K_eff. non-unitary P Non-trivial NSI & LFV adopted in oscillation analyses 3
4 Oscillation parameters Preliminary 2013 update of Phys. Rev. D 86, (2012) w/o recent T2K 4
![Preliminary 2013 LBL+SOL+KL + REACTOR arxiv:1310.6732 [hep-ex]. DayaBay 217-day S.](/docs-images/81/82685483/images/5-0.jpg "Seo s t alk at TAUP 2013, RENO 402-day + ATM Courtesy of Tortola non-trivial info on CP phase with new")
5 Preliminary 2013 LBL+SOL+KL + REACTOR arxiv: [hep-ex]. DayaBay 217-day S. Seo s t alk at TAUP 2013, RENO 402-day + ATM Courtesy of Tortola non-trivial info on CP phase with new T2K result
6 ORIGIN OF NEUTRINO MASS & SEESAW fermion exchange TYPE I Minkowski 77 Gellman Ramond Slansky 80 Glashow, Yanagida 79 Mohapatra Senjanovic 80 Lazarides Shafi Weterrich 81 Schechter-Valle, 80 & 82 Scalar-exchange TYPE II Schechter-Valle 80/82 SCALE Number & gauge properties of messengers MECHANISM LOW-SCALE SEESAW FLAVOR STRUCTURE Mohapatra-Valle 86 Akhmedov et al PRD53 (1996) 2752 Malinsky et al PRL95(2005) Bazzocchi et al, PRD81 (2010)
7 SUSY ORIGIN OF NEUTRINO MASS sneutrino sneutrino Masiero & Valle, PLB251 (1990) 273 Bhattacharyya & Pal, PRD82 (2010) EFF. BILINEAR RPV SUSY ATM SCALE SUSY-SEESAW SOLAR SCALE RADIATIVE Diaz et al PRD68 (2003) , PRD62 (2000) PRD65 (2002) ; PRD61 (2000) Bazzocchi et al JHEP 01 (2013) 033 arxiv:
8 LIGHTEST NEUTRALINO DECAYS: PROBING LHC De Campos et al Phys.Rev. D86 (2012) PRD82 (2010) & JHEP 0805:048, 2008 Lightest neutralino decay correlates with atm angle Lightest neutralino decay length 8
9 Sectors are separated by an extra Abelian Zn CHARGED LEPTONS THE FLAVOR PROBLEM A4 Babu et al PLB552 (2003) 207 Hirsch et al PRD69 (2004) Tri-BiMaximal ansatz Harrison, Perkins, Scott 2000 Altarelli, Feruglio
10 arxiv: STRIKING CORRELATION 10
11 A new way to relate Quarks to leptons? FLAVOR King et al GUT Phys. Lett. B 724 (2013) Morisi et al Phys.Rev. D88 (2013)
12 OSCILLATION PARAMETER CORRELATIONS Boucenna et al PhysRevD Phys. Lett. B 724 (2013) King et al Dorame, et al : 12
13 FLASY2011 FLASY2012 FLASY2013 Gflavor Fortsch.Phys. 61 (2013) Deviation of TBM Ishimori,etal Prog Theor Phys Suppl 183 (2010) 1 change ansatz: Albright,Dueck,Rodejohann Nilles, Morisi, JV Z. fur Phys, 2012 Anarchy Donoghue et al PRD73 Hall,Murayama,Weiner,PRL Altarelli, Feruglio,Masina,JHEP Holthausen et al BI-LARGE Boucenna,M,Tortola,Valle PRD86 (2012) Ding, Morisi, JV PRD (2013)
14 Bi-large mixing & Cabibbo angle reactor seeds solar & atm Abelian Flavor Models Boucenna et al, Phys. Rev. D 86, (R) Ding, et al Phys.Rev. D87 (2013) Roy, Singh,..arXiv:
15 OSCILLATION PARAMETER CORRELATIONS Boucenna et al PhysRevD Phys. Lett. B 724 (2013) King et al Dorame, et al : 15
16 TESTING NEUTRINO SPECTRA W/ NU-LESS Double Beta Decay King et al : Phys. Lett. B 724 (2013) F lavor S ensitivity DBD lower bounds Dorame et al NPB861 (2012) Dorame et al PhysRevD
17 Neutrinos affect the CMB and large scale structure in the Universe are fundamental in the synthesis of light elements can probe the Universe at much earlier epochs than photons explaining e.g. origin of dark matter... BIG-BANG
18 SNEUTRINO-like WIMP instead of neutralino DM Arina et al PRL101 (2008) Bazzocchi, Cerdeno, Munoz, J.V., PRD81 (2010) Inverse seesaw susy spectrum 18 18
19 DM STABILITY ACCIDENT? Lavoura, Morisi, JV JHEP 1302(2013) 118 Stable Non-SUSY WIMP from FLAVOUR SYMMETRY Z2 PARITY HIGGS PORTAL DIRECT DETECTION 19
20 DARK MATTER MAJORONS Consistency with CMB Berezinsky, Valle PLB318 (1993) 360 Lattanzi & Valle, PRL99 (2007) Esteves et al, PRD 82, (2010) Bazzocchi & al JCAP 0808 (2008) 013 Lattanzi et al PRD88 (2013)
21 Gamma line from decaying Gravitino dark matter decays suppressed by Planck mass & smallness of m-nu chosen to fit neutrino osc. data Restrepo et al PRD85 (2012) LHC relic abundance + LHC searches excluded by gamma line Egret & Fermi-LAT 21
22 OSCILLATIONS ROBUST... PHASE, SPECTRUM, OCTANT, NSI? ORIGIN OF NEUTRINO MASS : which MESSENGER? NEUTRINO PROPERTIES : LHC? FLAVOR PATTERN: anarchy or SYMMETRY? DARK MATTER relates to NEUTRINOS? DARK MATTER why STABLE? NON-SUSY WIMP? MAJORON & GRAVITINO as DECAYING DARK MATTER? 22
23 謝謝 23
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