Neutrino Pre-Town Meeting This is a town meeting: make your voice heard!

Nov , 2006Neutrino Pre-Town Meeting What we hope to do at the breakout sessions - The Agenda Discover and hear about the various ideas for current and future research Collect these ideas and try to uncover common themes Begin discussions about the given section of a white paper All slides are open to modification and input: As the discussion proceeds, we’ll try to collect our comments here.

Nov , 2006Neutrino Pre-Town Meeting Neutrino Physics is: Nuclear PhysicsParticle Physics AstrophysicsCosmology And probably others as well. But it is the NP Long range plan we are trying to influence.

Nov , 2006Neutrino Pre-Town Meeting Key Goals Want to deliver an effective message to the Town Meeting in January We need to: –Identify a coherent set of physics goals –Articulate why the research is nuclear physics and should be supported by NP –Indicate why the next 5 years are critical to this research –Identify critical needs

Neutrino Pre-Town Meeting This is a town meeting: make your voice heard! Neutrino Mass, Charge Conjugation, Lepton Flavor Violation Working Group Conveners: Steve Elliott/Guido Drexlin

Nov , 2006Neutrino Pre-Town Meeting Our working group includes, but is not necessarily limited to: How do we: determine the masses of the neutrinos? their charge-conjugation properties? determine if Lepton number conservation is violated?

Nov , 2006Neutrino Pre-Town Meeting Beta Decay Why Nuclear Physics? Nuclear decay process Fundamental particle participating in nuclear transition Traditional nuclear-physics experimental techniques Why now? Some experiments are being built Other experiments need R&D support

Nov , 2006Neutrino Pre-Town Meeting Beta Decay: representative list Tritium - KATRIN, NEXTEX (Abstract) 187 Re - MARE Theory: weak interaction descriptions, non-SM extensions

Nov , 2006Neutrino Pre-Town Meeting Double-Beta Decay Why Nuclear Physics? Nuclear decay process Fundamental particle participating in nuclear transition - the characteristics of that particle are critical to the nuclear process Backgrounds result from nuclear processes, thus experimenters require NP understanding Traditional nuclear-physics experimental techniques Important nuclear theory component Why now? Some experiments are being built Other experiments need R&D support Critical needs Underground laboratory

Nov , 2006Neutrino Pre-Town Meeting Double-Beta Decay: Representative list 48 Ca (CANDLES) 76 Ge (Gerda, Majorana) 82 Se (NEMO) 100 Mo (NEMO, MOON) 116 Cd (COBRA, … ) 130 Te (CUORE, COBRA) 136 Xe (EXO) 150 Nd (SNO+) Theory: nuclear matrix elements, RH currents, phenomenology

Nov , 2006Neutrino Pre-Town Meeting Other neutrino mass techniques IceCube (Abstract)

Nov , 2006Neutrino Pre-Town Meeting Related Technologies Low background counting facility (Abstract) Muon induced backgrounds (Abstract)

Nov , 2006Neutrino Pre-Town Meeting Dark Matter Why Nuclear Physics? Traditional nuclear-physics experimental techniques Backgrounds result from nuclear processes, thus experimenters require NP experience Important nuclear theory component Why now? Some experiments are being built Other experiments need R&D support Critical Needs Underground laboratory

Nov , 2006Neutrino Pre-Town Meeting Dark Matter: representative list Ne (CLEAN/DEAP) (Abstract) Si (CDMS) Ge (CDMS) Ar (CLEAN/DEAP, WARP) Xe (XENON, Zeplin) Theory: particle physics, cosmology

Nov , 2006Neutrino Pre-Town Meeting (Abstract)

Nov , 2006Neutrino Pre-Town Meeting

Nov , 2006Neutrino Pre-Town Meeting

Nov , 2006Neutrino Pre-Town Meeting