and Neutrino Factory 2004 based on Rob Fardon
and Neutrino Factory 2004, based on Rob Fardon, A. E. N. , Neal Weiner; astro-ph/0309800 David B. Kaplan, A. E. N. , Neal Weiner; hep-ph/0401099 Kathryn Zurek, hep-ph/0405141 Kiyoshi Shiraishi, unpublished
1998, First Convincing evidence for Physics Beyond the Standard Model from Super. K, evidence for atmospheric neutrino oscillations “Breakthrough of the Year” is the supernovae evidence for the But, the acceleration of the universe Einstein was wrong about having blundered? (Cosmological Constant? ) “Why Now” and finetuning are evidence for the Anthropic Principle?
Strong Evidence for two kinds: 1. 23% Dark Matter -> some garden variety pressureless clumpy fluid 2. 73% “Dark Energy” -> exotic negative pressure smooth substance usually attributed to the energy of the vacuum� energy density which does not dilute with expansion and is therefore equivalent to Einstein’s cosmological constant. I will assume this is zero. sometimes assumed to be some weird dynamical “quintessence” substance with equation of state parameter w near -1 which nevertheless does not clump (not your typical nonrelativistic stuff)
“Smooth, Dark, Tension” Sean Carroll • • Negative Pressure=Tension Smooth Tension= Oxymoron? “Normal” Stuff under tension prefers to Clump Weird particle physics counterexamples: 1 vacuum energy la slowly rolling scalar field (m~H-1~ 10 -33 e. V) dfrustrated network of strings/domain walls 4 relativistic, freely streaming particles
After Six Years of Surprises, Do we Almost Completely Understand Neutrinos Now? Flavor Composition of n Mass Eigenstates q 13 Absolute mass scale? CP? Majorana or Dirac? LSND outlier?
Why recent Concordance in the neutrino oscillation Industry? Neutrinos are Special! Expect exotic physics to be discovered there! Window on the Dark Sector! Can mix with ‘dark’ fermions (aka sterile neutrinos) Can thus experience ‘dark forces’ much more strongly than other particles Oscillations are sensitive to tiny GUT suppressed operators (standard seesaw) Environment dependence of oscillations is sensitive to new millimeter range forces which are subgravitational strength for other particles
Beyond the n Standard Model Subject still in experimental youth Neutrino oscillations offer incredible sensitivity to new forces, high scales, ultraweak interactions, new states Conventional Wisdom about neutrinos, neutrino expts. has always been wrong!
Coincidences? Density of “Dark Energy” ~ (2 10 -3 )4 e. V 4 Solar Neutrino Mass 2 splitting ~ (4 10 -3 )2 e. V 2 Atmospheric Neutrino Mass 2 splitting ~ (3 10 -2 ) 2 e. V 2 Convincing evidence for Dark Energy found in 1998 Convincing evidence for Neutrino Oscillations found in 1998 -3 Low Scale SUSY gravitino mass ~ 10 e. V
More Coincidences. Why so complicated?
Can dark energy be related to something we know? Dark Matter? We know scaling behavior of dark matter from large scale structure. Dark energy currently scales very differently. Scaling behavior of dark energy must have recently changed (Why Now? ) Neutrinos? Could neutrino energy density scale like dark energy? Requires neutrino ‘mass’ to increase with scale factor Isn’t varying neutrino mass crazy? No
Varying ‘Mass’ is Everywhere! Index of refraction KS regeneration Quasi particles in condensed matter MSW effect All Standard Model fermion mass terms depend on value of Higgs scalar which can vary (slightly) All known masses depend on environment The issue is not ‘whether’, but ‘how much’ neutrino mass should vary !
A simple Mass. Varying. Neutrino Model Assume “Dark Sector” (= unknown particles with no standard Model charges) contains 1 A scalar field A 1 A fermion field n 1 A Yukawa coupling A n n 1 A scalar potential V ( A ) Assume “Our sector” contains 1 Active Neutrinos n 1 Higgs Field H Allow tiny (y =O (10 -12) ) coupling y H n n æNeutrino mass matrix. ( 0 y. H A )
Neutrino Masses vary as A n Neutrino mass matrix n ( n n 0 y. H A -1 ) 2 For large <A> light neutrino mass is ( y H) / A Assume V ( A ) slowly increasing function of A. V is then slowly decreasing function of the light neutrino mass V(A (mn) ) ~ mn (1+w)/ w
Neutrino mass increases adiabatically as neutrino density dilutes Combined neutrino + scalar potential energy decreases slowly
What is the Scale? We have 2 pieces of evidence suggesting a milli-e. V scale for new physics. This is also the inverse cosmic neutrino spacing. A milli-e. V scale for the A potential (and mass) leads to Dark Energy Contrast with ‘cosmon’ type quintessence model, which requires a mass scale of 10 -33 e. V.
Smoothness of Ma. Va. N Dark Energy • When n’s go nonrelativistic, they gravitationally clump at large scales • Ma. Va. N’s go nonrelativistic very late (z= a few) • Ma. Va. N’s get lighter and more relativistic inside clumps => ‘anti-clumping mechanism’ • Dark energy much smoother than neutrinos V ~ (nn) (1+w)
Sterile Neutrinos? Sterile neutrino mass increasing function of neutrino density Mixing with sterile neutrino decreasing function of neutrino density Simple to reconcile sterile neutrino with BBN F mass always much heavier than temperature May similarly evade Supernovae bounds
Can we test Ma. Va. N Dark Energy? Cosmological tests of neutrino mass from large scale structure: Ma. Va. N mass was much lighter at high redshift. Model independent relation: mn= (1+w) V/nn (V= dark energy density) No terrestrial sources of high scalar neutrino density (neutrino density weighted by (m/E)), relative to cosmological, other than nuclear fireball. Main interesting astrophysical source of high scalar neutrino density is supernova. Generic tests difficult, not impossible.
A should have coupling to matter Loop suppressed and/or Planck/String scale suppressed Possible very interesting terms:
• Recent unofficial, preliminary analysis of Super. K atmospheric neutrinos by Kiyoshi Shiraishi assuming no oscillations in air fits all data well • Very weak (consistent with LSND? ) upper bound on mass squared difference in rock from contained, partially contained events, K 2 K • reanalysis of upward through going and upward stopping muons underway, probably yields best upper bound on Dm 2 in rock
Conventional Wisdom: need > 3 neutrinos to get 3 independent masses squared, and oscillations involving extra dark states constrained by Bugey, CDHS, Cosmology, and Supernova, so LSND must be wrong Constraints on Standard Neutrinos Constraints from oscillations in High Density Material only
To Do: Theorists Model building exploration Ma. Va. N consequences for Supernova How much room for non standard environment dependence in Solar/atmospheric/terrestial neutrino oscillations? Consequences for flavor dependence/energy spectrum of astrophysical neutrino sources Early Universe cosmology of acceleron More general constraints on sterile neutrinos from supernovae, cosmology
To Do: Experimentalists Document and consider environment of neutrino path in neutrino oscillation experiments Consider q 13 measurements in reactor experiments with pathlength in air and in rock Consider environment of neutrinos in direct mass search and 0 nbb measurements Short baseline experiments to search for heavier sterile neutrinos with small mixing angles; consider varying density of material in neutrino path
Effects of environment in neutrino oscillations? 0 nbb decay depends on density of source? Tritium endpoint searches for absolute n mass depends on density of source? Cosmologically “impossible” sterile neutrinos? Cosmologically “inconsistent” neutrino masses? A Mini. Boo. NE signal for nm disappearance or ne appearance
- Slides: 27
