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Neutrino Physics

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Probe to High Energies. Effects of physics beyond the SM as ... EGRET down to =2 10-8cm-2sec-1. GLAST down to ~10-11cm-2sec-1. Neutrinos/km3: ~4 10-10cm-2sec-1 ... – PowerPoint PPT presentation

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Title: Neutrino Physics


1
Neutrino Physics
  • Hitoshi Murayama (BerkeleyIPMU)
  • NNN 2007, Hamamatsu
  • Oct 3, 2007

2
Outline
  • Past Why Neutrinos?
  • Present Era of Revolution
  • Near Future Bright Prospect
  • Big Questions Need Synergies
  • Astrophysical Probe
  • Conclusion

3
Past
  • Why Neutrinos?

4
Probe to High Energies
  • Effects of physics beyond the SM as effective
    operators
  • Can be classified systematically (Weinberg)

5
Unique Role of Neutrino Mass
  • Lowest order effect of physics at short distances
  • Tiny effect (mn/En)2(0.1eV/GeV)21020!
  • Inteferometry (i.e., Michaelson-Morley)
  • Need coherent source
  • Need interference (i.e., large mixing angles)
  • Need long baseline
  • Nature was kind to provide all of them!
  • neutrino interferometry (a.k.a. neutrino
    oscillation) a unique tool to study physics at
    very high scales
  • Not entirely surprising (in retrospect) that
    neutrino mass was the first evidence for physics
    beyond standard model

6
Ubiquitous Neutrinos
They must have played some important role in the
universe!
7
Astrophysical Probe
  • Neutrinos unhindered by the entire star, dusts,
    CMB, galactic intergalactic B, even last
    rescattering surface
  • Possible probe into
  • Core of stars (Sun, supernovae, GRB)
  • Near blackholes (AGN)
  • Dark Matter (Sun, galactic center, subhalo)
  • Cosmology?

8
Present
  • Era of Revolution

9
The Data
  • Evidence for oscillation
  • Indisputable
  • Atmospheric
  • Solar
  • Reactor
  • strong
  • Accelerator (K2K)
  • And we shouldnt forget
  • unconfirmed
  • Accelerator (LSND)

10
SuperKamiokande Atmospheric ? disappear
Downwards ??s dont disappear
1/2 of upwards ??s do disappear
11
SNOSolar ? transform in flavor
2/3 of ?es ? ????
12
KamLANDReactor neutrinos do oscillate!
?Proper time ?
L0180 km
13
What we learned
  • Lepton Flavor is not conserved
  • Neutrinos have tiny mass, not very hierarchical
  • Neutrinos mix a lot
  • the first evidence for
  • demise of the Minimal Standard Model
  • Very different from quarks

14
The Big Questions
  • What is the origin of neutrino mass?
  • Did neutrinos play a role in our existence?
  • Did neutrinos play a role in forming galaxies?
  • Did neutrinos play a role in birth of the
    universe?
  • Are neutrinos telling us something about
    unification of matter and/or forces?
  • Will neutrinos give us more surprises?
  • Big questions ? tough questions to answer

15
Immediate Questions
  • Dirac or Majorana?
  • Absolute mass scale?
  • How small is q13?
  • CP Violation?
  • Mass hierarchy?
  • Is q23 maximal?

16
Future
  • Bright Prospect

17
Immediate Questions
  • Dirac or Majorana?
  • Absolute mass scale?
  • How small is q13?
  • CP Violation?
  • Mass hierarchy?
  • Is q23 maximal?

18
Extended Standard Model
  • Massive Neutrinos ? Minimal SM incomplete
  • How exactly do we extend it?
  • Abandon either
  • Minimality introduce new unobserved light
    degrees of freedom (right-handed neutrinos)
  • Lepton number abandon distinction between
    neutrinos and anti-neutrinos and hence matter and
    anti-matter
  • Dirac or Majorana neutrino
  • Without knowing which, we dont know how to
    extend the Standard Model
  • KATRIN, 0???, Large Scale Structure

19
Immediate Questions
  • Dirac or Majorana?
  • Absolute mass scale?
  • How small is q13?
  • CP Violation?
  • Mass hierarchy?
  • Is q23 maximal?

20
T2K (Tokai to Kamioka)
21
Immediate Questions
  • Dirac or Majorana?
  • Absolute mass scale?
  • How small is q13?
  • CP Violation?
  • Mass hierarchy?
  • Is q23 maximal?
  • LSND? Sterile neutrino(s)? CPT violation?

22
LMA confirmed by KamLAND
  • Dream case for neutrino oscillation physics!
  • Dm2solar within reach of long-baseline expts
  • Even CP violation may be probable
  • Possible only if
  • Dm122, s12 large enough (LMA)
  • q13 large enough

23
q13 decides the future
  • The value of q13 crucial for the future of
    neutrino oscillation physics
  • Determines the required facility/parameters/baseli
    ne/energy
  • sin22q13gt0.01 ? conventional neutrino beam
  • sin22q13lt0.01 ? ? storage ring, ? beam
  • Two paths to determine q13
  • Long-baseline accelerator T2K, NO?A
  • Reactor neutrino experiment 2?CHOOZ, Daya Bay

24
NO?AFermilab to Minnesota
25kt
NOnA
MINOS
L810km
25
Daya Bay
Empty detectors moved to underground halls
through access tunnel. Filled detectors swapped
between underground halls via horizontal tunnels.
Ling Ao Near 500 m from Ling Ao Overburden 98 m
Ling Ao-ll NPP (under const.)
Ling Ao NPP
Entrance portal
Daya Bay NPP
Total tunnel length 2700 m
26
3? sensitivity on sin2 2?13
27
T2K vs NO?A
  • LBL ????e appearance
  • Combination of
  • sin22?13
  • Matter effect
  • CP phase ?

95CL resolutionof mass hierarchy
28
Accelerator vs Reactor
Reactor w 100t (3 yrs) T2K T2K (5yr,n-only)
Reactor w 10t (3 yrs) T2K
90 CL
90 CL
Reactor experiments can help in Resolving the
?23 degeneracy (Example sin22?23 0.95
0.01)
Reactor w 100t (3 yrs) Nova Nova only (3yr
3yr) Reactor w 10t (3yrs) Nova
90 CL
McConnel Shaevitz, hep-ex/0409028
29
My prejudice
?23
?12
?13
  • Lets not write a complicated theory
  • The only natural measure for mixing angles is the
    group-theoretical invariant Haar measure
  • KolmogorovSmirnov test 64
  • sin2 2q13gt0.04 (2s)
  • sin2 2q13gt0.01 (99CL)

30
T2KK
CP-violation may be observed in neutrino
oscillation!
31
Big Questions
  • Need Synergies

32
Immediate Questions
  • Dirac or Majorana?
  • Absolute mass scale?
  • How small is q13?
  • CP Violation?
  • Mass hierarchy?
  • Is q23 maximal?

33
What about the Big Questions?
  • What is the origin of neutrino mass?
  • Did neutrinos play a role in our existence?
  • Did neutrinos play a role in forming galaxies?
  • Did neutrinos play a role in birth of the
    universe?
  • Are neutrinos telling us something about
    unification of matter and/or forces?
  • Will neutrinos give us more surprises?
  • Big questions ? tough questions to answer

34
Seesaw Mechanism
  • Why is neutrino mass so small?
  • Need right-handed neutrinos to generate neutrino
    mass

, but nR SM neutral
To obtain m3(Dm2atm)1/2, mDmt, M310141015 GeV
35
Leptogenesis
  • You generate Lepton Asymmetry first. (Fukugita,
    Yanagida)
  • Generate L from the direct CP violation in
    right-handed neutrino decay
  • L gets converted to B via EW anomaly
  • ? More matter than anti-matter
  • ? We have survived The Great Annihilation
  • Despite detailed information on neutrino masses,
    it still works (e.g., Bari, Buchmüller, Plümacher)

36
Origin of Universe
V(?)
  • Maybe an even bigger role
  • Microscopically small Universe at Big Bang got
    stretched by an exponential expansion (inflation)
  • Need a spinless field that
  • slowly rolls down the potential
  • oscillates around it minimum
  • decays to produce a thermal bath
  • The superpartner of right-handed neutrino fits
    the bill
  • When it decays, it produces the lepton asymmetry
    at the same time
  • (HM, Suzuki, Yanagida, Yokoyama)
  • Neutrino is mother of the Universe?

?
log R
t
37
LHC/ILC may help
  • LHC finds SUSY
  • ILC measures masses precisely
  • If both gaugino and sfermion masses unify, there
    cant be new particles lt 1014GeV except for
    gauge-singlets

38
Plausible scenario
  • 0??? found
  • LHC discovers SUSY
  • ILC shows unification of gaugino and scalar
    masses
  • Dark matter concordance between collider,
    cosmology, direct detection
  • CP in ?-oscillation found
  • Lepton flavor violation limits (??e?, ??e
    conversion, ???? etc) improve or discovered
  • Tevatron and EDM (e and n) exclude Electroweak
    Baryogenesis
  • CMB B-mode polarization gives tensor mode r0.16

If this happens, we will be led to
believe seesawleptogenesis (Buckley, HM)
39
Neutrinos as Astrophysical Probe
40
(No Transcript)
41
Dark Matter
  • Indirect detection of galactic dark matter
  • From the Sun, Galactic Center, Subhalos

42
??s ??s
  • EGRET down to ??2?10-8cm-2sec-1
  • GLAST down to ??10-11cm-2sec-1
  • Neutrinos/km3 ??4?10-10cm-2sec-1
  • The catch
  • GLASTgtGeV
  • Icecubegt100GeV?
  • Cross-correlation between ??s ??s gives us
    understanding of the source

Buckley, Freese, HM, Spolyar, Sourav
43
Dark Energy with Neutrinos?
  • Supernova relic neutrinos come from cosmological
    distances
  • Its spectrum redshifted and superimposed
  • Depends not only supernova rates and spectra, but
    also on the geometry of space
  • Count Type-II_at_SNAP
  • In principle, sensitive to Dark Energy
  • HyperGADZOOKS!

44
Conclusions
  • Neutrino oscillation a unique tool to probe
    (very) high-energy world
  • Era of revolution
  • sin2 2?13 decides the future of LBL expts
  • My prejudice ?13 is large
  • Reactor accelerator LBL expts complementary
  • To understand big questions we need a diverse
    set of experiments
  • Neutrinos are also unique astrophysical probes
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