Updating the Status of Neutrino Physics

Transcription

1 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.

2 Atmospheric zenith distribution Maltoni, Schwetz, Tortola and JV PRD67 (23) Φ µ ( -3 cm -2 s - sr - ) # events SK sub-gev (µ) SK stop (µ) cos θ cos θ SK multi-gev (µ) SK thru (µ) SK-489 No oscillations Best [d s =.92, d µ =.4] Active [d s =., d µ =.] Sterile [d s =., d µ =.] MACRO thru (µ) cos θ String Phenomenology 23, Durham p.2

3 atmospheric neutrino parameters- sterility rejection 6 Maltoni et al PRD67 (23) 3 5 hep-ph/27227 m 2 3 [-3 ev 2 ] H sin 2 θ 23 light-dark or normal/inverted symmetry String Phenomenology 23, Durham p.3

4 How robust are atmospheric oscillations? very good contained atm-fit, Gonzalez-Garcia et al, PRL 82 (999) # events Φ µ ( -3 cm -2 s - sr - ) SK sub-gev (µ) SK stop (µ) cos θ SK multi-gev (µ) SK thru (µ) cos θ No Oscillations Best Fit, OSC Best Fit, NSI Best Fit, Hybrid MACRO thru (µ) cos θ String Phenomenology 23, Durham p.4

5 non-standard interactions vs atm data Fornengo et al, PRD 65 (22) 3 [hep-ph/843]. χ Hybrid OSC 99% CL 95% CL 9% CL -3-2 m 2 [ev 2 ] 2 ± ε χ 2 5 Hybrid OSC 5 99% CL 95% CL 9% CL sin 2 2θ 2 ± ε, atm bounds on FC and NU nu-interactions String Phenomenology 23, Durham p.5

6 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/ 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

7 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 % C.L. ( d.o.f.) Global Reactor KamLAND in contrast to atmospheric, solar mixing significantly non-maximal 5 bi-maximal models rejected m 2 [ev 2 ] - tan 2 (θ) String Phenomenology 23, Durham p.7

8 do we understand the Sun?.8 L =km noise=% Density r/r sun String Phenomenology 23, Durham p.8

9 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 E [MeV] 5 5 E [MeV] 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

10 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 sin 2 2θ LSND Maltoni et al NPB643 (22) 32 upd of PRD65 (22) 934 ATM LSND SOL String Phenomenology 23, Durham p.

11 Cosmology closes in on LSND m 2 LSND [ev2 ] H 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.

12 Three neutrino parameters in a nut shell upg of Maltoni et al, PRD67 (23) 3 & PRD 67 (23) 933, upd of PRD63 (2) { m 2 2, m2 3 } [ev2 ] -3-4 H H H H {sin 2 θ 2, sin 2 θ 23 } sin 2 θ χ { m 2 2, m2 3 } [ev2 ] {sin 2 θ 2, sin 2 θ 23 } sin 2 θ 3 String Phenomenology 23, Durham p.2

13 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 νν ν ν ν 2 3 ν 2 3 String Phenomenology 23, Durham p.3

14 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) masses: 2 angles: and 2 CP violating phases: String Phenomenology 23, Durham p.4

15 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 String Phenomenology 23, Durham p.5

16 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

17 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

18 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

19 Theory ideas String Phenomenology 23, Durham p.9

20 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

21 neutrino unification: large-scale seesaw /ev vs. Log /GeV Babu, Ma and Valle, PLB552 (23) 27 neutrino masses unify as they run up 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

22 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

23 LSP decay length [cm]: BRPV from Bartl et al NPB 6 (2) ev ev ev [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

24 neutrino mixing angles in BRPV mixings in terms of RPV ratios, e,g, atm mixing - -2 vs LSP decay properties correlate with angles neutralino Porod et al PRD63 (2) / vs stop decays Restrepo, Porod & Valle, PRD64 (2) 55 slepton decays M. Hirsch et al, PRD66 (22) 956 String Phenomenology 23, Durham p.24

25 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 valle/talks/talks.html String Phenomenology 23, Durham p.25