Updating the Status of Neutrino Physics J. W. F. Valle IFIC-CSIC/U. Valencia Based on hep-ph/36 and hep-ph/3792 String Phenomenology 23, Durham p.
Atmospheric zenith distribution Maltoni, Schwetz, Tortola and JV PRD67 (23) 3 5 25 Φ µ ( -3 cm -2 s - sr - ) # events 4 3 2 SK sub-gev (µ) - -.5.5 SK stop (µ) - -.8 -.6 -.4 -.2 2 5 5.8 3.6 2.4.2 - -.5.5 4 cos θ cos θ SK multi-gev (µ) SK thru (µ) - -.8 -.6 -.4 -.2 6 5 4 3 2 SK-489 No oscillations Best [d s =.92, d µ =.4] Active [d s =., d µ =.] Sterile [d s =., d µ =.] MACRO thru (µ) - -.8 -.6 -.4 -.2 cos θ String Phenomenology 23, Durham p.2
atmospheric neutrino parameters- sterility rejection 6 Maltoni et al PRD67 (23) 3 5 hep-ph/27227 m 2 3 [-3 ev 2 ] 4 3 2 H.2.4.6.8 sin 2 θ 23 light-dark or normal/inverted symmetry String Phenomenology 23, Durham p.3
How robust are atmospheric oscillations? very good contained atm-fit, Gonzalez-Garcia et al, PRL 82 (999) 322 5 4 25 2 # events Φ µ ( -3 cm -2 s - sr - ) 3 2.8.6.4.2 SK sub-gev (µ) -.8 -.4.4.8 SK stop (µ) - -.8 -.6 -.4 -.2 cos θ 5 5 4 3 2 SK multi-gev (µ) -.8 -.4.4.8 SK thru (µ) - -.8 -.6 -.4 -.2 cos θ 6 5 4 3 2 No Oscillations Best Fit, OSC Best Fit, NSI Best Fit, Hybrid MACRO thru (µ) - -.8 -.6 -.4 -.2 cos θ String Phenomenology 23, Durham p.4
non-standard interactions vs atm data Fornengo et al, PRD 65 (22) 3 [hep-ph/843]. χ 2 5 5 Hybrid OSC 99% CL 95% CL 9% CL -3-2 m 2 [ev 2 ] 2 ± 3 + 2 + ε χ 2 5 Hybrid OSC 5 99% CL 95% CL 9% CL.6.7.8.9 sin 2 2θ 2 ± 3 + 2 + ε, atm bounds on FC and NU nu-interactions String Phenomenology 23, Durham p.5
Solar + KamLAND reactor results -3 Maltoni, Schwetz & JV, PRD67 (23) 933 [hep-ph/2229] m 2 [ev 2 ] -4-5 H first 45-days data support oscillation hypothesis critique of various analyses S. Pakvasa and JV hep-ph/36-6.2.4.6.8 sin 2 2θ -3 combining with solar neutrino data sample rules out non-lma-msw solutions oscilllations happen inside the sun! m 2 [ev 2 ] -4 H -5 - tan 2 θ String Phenomenology 23, Durham p.6
Solar + KamLAND results -3 Maltoni, Schwetz, JV, PRD67 (23) 933 consistency with Poisson method m 2 [ev 2 ] -4 H enormous progress wrt pre-kamland -5 - tan 2 θ 2 χ 2 5 99.73% C.L. ( d.o.f.) Global Reactor KamLAND in contrast to atmospheric, solar mixing significantly non-maximal 5 bi-maximal models rejected -6-5 -4-3 m 2 [ev 2 ] - tan 2 (θ) String Phenomenology 23, Durham p.7
do we understand the Sun?.8 L =km noise=% Density.6.4.2..2.3.4.5.6.7.8.9 r/r sun String Phenomenology 23, Durham p.8
Robustness of MSW plot Burgess et al, Astrophys.J.588:L65,23 [hep-ph/2994].6 LMA noise=4% noise=8% neutrino propagation strongly affected by density noise Balantekin et al 95 Nunokawa et al NPB472 (996) 495 Burgess et al 97 Pee.5.4.3 5 5 E [MeV] 5 5 E [MeV] 5 5 2 E [MeV] -3 Without noise L= km, noise=free substantial distortion m 2 [ev 2 ] -4 H H lower possible -5 - tan 2 θ - tan 2 θ String Phenomenology 23, Durham p.9
LSND hints of neutrino conversions also from the detection of accelerator-produced neutrinos in the LSND experiment 4-nu models Peltoniemi, JV, NPB46, 49 (993) Peltoniemi, Tommasini and JV, PLB298 (993) 383 m 2 LSND [ev2 ] LSND DAR Caldwell-Mohapatra PRD48 (993) 325 LSND global barely possible at 3 3 2 sin 2 2θ LSND Maltoni et al NPB643 (22) 32 upd of PRD65 (22) 934 ATM LSND SOL String Phenomenology 23, Durham p.
Cosmology closes in on LSND m 2 LSND [ev2 ] H - -3-2 sin 2 2θ LSND 2df + WMAP + HST + SNIa Schwetz et al hep-ph/3532 Spergel et al, astro-ph/3229; Hannestad, astro-ph/3376; Elgaroy & Lahav, astro-ph/3389 String Phenomenology 23, Durham p.
Three neutrino parameters in a nut shell upg of Maltoni et al, PRD67 (23) 3 & PRD 67 (23) 933, upd of PRD63 (2) 335-2 { m 2 2, m2 3 } [ev2 ] -3-4 H H H H -5.2.4.6.8-3 -2 - {sin 2 θ 2, sin 2 θ 23 } sin 2 θ 3 2 5 χ 2 5-6 -5-4 -3-2 -.2.4.6.8-3 -2 - { m 2 2, m2 3 } [ev2 ] {sin 2 θ 2, sin 2 θ 23 } sin 2 θ 3 String Phenomenology 23, Durham p.2
minimal set of basic parameters 3 angles KM-like phase oscillations 2 Majorana phases 23=atm 2=sol 3=reac Schechter and JV, PRD22 (98) 2227, D23(98) 666 both appear in leptogenesis [ev] Hierarchical spectrum [ev] 2 Degenerate spectrum - -2-3 - -4-2 νν ν ν ν 2 3 ν 2 3 String Phenomenology 23, Durham p.3
and the neutrino spectra (mass mechanism) given that neutrinos are massive, one expects to occur with an amplitude governed by the average mass parameter n d u d W d u u e- p ν = ν c e- W parametrizing as in n d u d d u u p Schechter and JV, PRD22 (98) 2227 3 masses: 2 angles: and 2 CP violating phases: String Phenomenology 23, Durham p.4
current laboratory tests of absolute neutrino mass Current sol-atm, and Tritium sensitivities thanks to Martin Hirsch Current neutrino oscillation data Upper limit for ev with factor Upper limit from Tritium experiments: uncertainty band ev normal versus inverse hierarchy Log /ev vs Log /ev - - -2-2 -3-3 -4-4 -4-3 -2 - -4-3 -2 - String Phenomenology 23, Durham p.5
Relevance of gauge theories majorana mass u u Schechter and JV, PRD 25 (982) 295 d d no such theorem for flavor violation! W νββ W e e ν ν String Phenomenology 23, Durham p.6
Perversity of nature? and Leptonic CP Violation Dirac CPV suppressed, since disappears when any Schechter and JV, PRD 2 (98) 39 Try harder String Phenomenology 23, Durham p.7
Neutrino Factories will probe and Cervera et al, De Rujula, Gavela, Hernandez Freund, Huber, Lindner, Albright et al, Barger et al... provided Non-Standard nu-intercations (NSI) can be rejected... Huber, Schwetz & JV PRL88 (22) 84 & PRD66, 36 (22) Huber & JV PLB523 (2) 5 String Phenomenology 23, Durham p.8
Theory ideas String Phenomenology 23, Durham p.9
basic dim-5 operator from Gravity Weinberg... from seesaw schemes Gell-Mann, Ramond, Slansky; Yanagida; Mohapatra, Senjanovic PRL44 (98) 9 Schechter, JV PRD22 (98) 2227; PRD25 (982) 774 String Phenomenology 23, Durham p.2
neutrino unification: large-scale seesaw /ev vs. Log /GeV Babu, Ma and Valle, PLB552 (23) 27 neutrino masses unify as they run up 2 3 4 5 6 7 8 9 2 3 4 Chankowski, Ioannisian, Pokorski and JV, PRL86 (2) 3488 solar & atm splittings from RGE common origin for neutrino and KM mixing maximal ; large & or maximal CP violation see also Grimus & Lavoura observable neutrino mass eg in cosmology, and decays observable Lepton Flavor Violation String Phenomenology 23, Durham p.2
bilinear R parity violation: weak-scale seesaw Diaz, Hirsch, Porod, Romao and JV, PRD68 (23) 39 [hep-ph/322]; PRD62 (2) 38 [Err-ibid. D65 (22) 99]; PRD6 (2) 773 weak-scale seesaw atm scale M= RPV SEESAW radiative nu-masses solar scale LOOPS - - String Phenomenology 23, Durham p.22
LSP decay length [cm]: BRPV from Bartl et al NPB 6 (2) 39... ev ev ev 3 4 5 6 7 8 9 [GeV] Mukhopadhyaya, Roy & Vissani; Chun & Lee; Choi et al; Datta et al any charged SUSY particles can be the LSP String Phenomenology 23, Durham p.23
neutrino mixing angles in BRPV mixings in terms of RPV ratios, e,g, atm mixing - -2 vs -3-4 5-2 -.5 LSP decay properties correlate with angles neutralino Porod et al PRD63 (2) 54 5.5 / vs...5 5 stop decays Restrepo, Porod & Valle, PRD64 (2) 55 slepton decays M. Hirsch et al, PRD66 (22) 956 String Phenomenology 23, Durham p.24
No Road Map to Theory of Neutrino Mass top-bottom vs bottom-up what is the mechanism? tree vs radiative B-L gauged vs ungauged... what is the scale? Planck scale: Strings? GUT scale,,... Intermediate scale: P-Q, L-R... Weak no theory of flavour are there sterile-nus? scale http://alpha.ific.uv.es/ valle/talks/talks.html String Phenomenology 23, Durham p.25