1 / 19

Exploring Neutrino Physics in Underground Laboratories: A Comprehensive Review

This review covers neutrino physics studies between 2005-2010, discussing various experiments like Solar, KamLAND, atmospheric, K2K, CHOOZ, and more. It delves into topics such as neutrino mass ranges, appearance signals, matter effects, adiabatic transitions, adiabatic transitions, and neutrinoless double beta decay. The text also highlights significant advancements, project proposals, and nuclear matrix elements using methods like QRPA and SM. Key discussions on small parameters, CP violation observables, majorana mass, and future directions in neutrino research are included.

red
Download Presentation

Exploring Neutrino Physics in Underground Laboratories: A Comprehensive Review

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 2005-2010 : Neutrino physics in underground labs ~ Carlos Pena Garay IAS UAM-IFT, Madrid

  2. The Neutrino Matrix :SM + n mass 3 s ranges: 1 s ranges: Solar + KamLANDAtmospheric + K2K CHOOZ thanks to Gonzalez-Garcia, Maltoni

  3. LSND vs KARMEN LSND : L=30 m, 20<E<60 MeV 3.5 to 7 s appearance signal depending on analysis 67 signal events in 1030 signal+background KARMEN : L=17.5 m, 20<E<60 MeV 15 events observed 15.8 background expected Church et al, hep-ex/0203023 Discussion : S. Pascoli, M. Sorel

  4. Known knows

  5. Known knows

  6. Where we are ? Test matter effects in solar neutrinos : - From vacuum averaged oscillations to adiabatic transitions- Daynight effectTest atmospheric oscillations : robustness of Dm232Improve precision Tests beyond SM physicsNeutrinos as astrophysical probes Valle’s talk, Halzen’s talk

  7. Known Unknows NH ? or IH ? q13 ?, d ? 4q23=p ? m? Majorana mass ?

  8. Hierarchy By matter effects in the 13 sector in atmospheric neutrinos, long baseline experiments, similar to matter effects determination in solar neutrinosq13 non zero break q13 – hierarchy degeneracyBy vacuum oscillations with d(Dm231)<Dm221valid even if q13=0 break q13 – hierarchy degeneracyBy high statistics short baseline reactor neutrino experimentsq13 not too smallBy matter effects in SupernovaBy neutrinoless double beta decay … Raffelt’s talk Discussion

  9. 4q23=p By solar osc. in atmospheric neutrinos, sub-GeV valid even if q13 =0 discrimination of octantBy atmospheric neutrinos, multi-GeVq13 nonzero discrimination of octantAccelerator neutrinos, MINOS : Non –maximal 3s detection if q23 is outsidethe ATM+K2K 90%CL (sin2q23<0.4) thanks to Gonzalez-Garcia, Maltoni, Winter

  10. q13 smallness All probes are sensitive to q13 (at different scales, with different sensitivities)2005-2010 hits : 1. MINOS more precise determination of the atmospheric splitting2. Double-CHOOZ sets the most stringent limit, unless atmospheric splitting is lower than expected. Discussion Solar + 2xKamLAND2xAtmospheric + K2K CHOOZMINOSDouble-CHOOZ

  11. 2010 null hypothesis: Preliminary! 3 s ranges: 1 s ranges: 1s determination of small parameters relevant in CP violation observables Solar + 2xKamLAND2xAtmospheric + K2K CHOOZMINOSDoble-CHOOZ thanks to Gonzalez-Garcia, Maltoni, Winter

  12. Mass scale Direct mass detection : KATRIN CosmologyNeutrinoless double beta decay Raffelt’s talk, Verde’s Discussion

  13. Majorana mass observed searching If observed : Neutrinos are MajoranaCan we learn anything more ?

  14. 0nbb 214Bi 214Bi ? Positive signal ? Klapdor et al (part of HM) 28.8 (6.9)->3-4s Bckg ~ 60 ev.

  15. Present Limits : Candidate Detector Present <m> (eV) nucleus type (kg yr) T1/20νββ (yr) 48Ca >9.5*1021 (76%CL) 76Ge Ge diode ~30 >1.9*1025 (90%CL) <0.39+0.17-0.28 82Se >9.5*1021 (90%CL) 100Mo >5.5*1022 (90%CL) 116Cd >7.0*1022 (90%CL) 128Te TeO2 cryo ~3 >1.1*1023 (90%CL) 130Te TeO2 cryo ~3 >2.1*1023 (90%CL) <1.1 - 2.6 136Xe Xe scint ~10 >1.2*1024 (90%CL) <2.9 150Nd >1.2*1021 (90%CL) 160Gd >1.3*1021 (90%CL)

  16. Projected/proposed

  17. nuclear matrix elements? Nuclear Physics methods : QRPA, SMTest QRPA : 20% variationTest SM ? Test QRPA-SM ?If positive signals : Test of models, but no model independent massCC n-nucleus interaction to measure many virtual transition in neutrinoless double beta Faessler et al, 2005 Volpe, 2005

  18. From Osc. Data :

  19. If no 0nbb If IH is correct, we need :a larger atmospheric neutrino exp.or a longer baseline in beam exp.Understanding of matrix elements(we don’t today)<0.01 eV sensitivity

More Related