Maori welcome

1
(No Transcript)
2
(No Transcript)
3
Maori welcome
4
(No Transcript)
5
Summary of Neutrino08

• Robert L. Flack

Thanks to the group and the graduate school for
jointly funding my attendance at the conference.
6
The conference was hosted by the University of
Canterbury, Christchurch, NZ.
http//www2.phys.canterbury.ac.nz/jaa53/index.htm

50 plenary and gt100 beer and pizza talks.
Therefore this is highly personal review of the
plenary talks.
This talk comes with a health warning the
words are a mixture of mine and the author and I
apologise if I misrepresent or misinterpret any
of the speakers.
7
Ernest Rutherford (Cecilia Jarlskog)
It is the 100th anniversary of the award of the
1908 Nobel Prize for chemistry to Ernest
Rutherford for his work on radioactivity.
He was born in Spring Grove, Nelson, New Zealand
in 1871. He attended Canterbury University and
his laboratory still exists and can be visited to
this day. Cecilia pointed out that although he
was working in England at the time he was not
proposed by any English physicists.
8
Properties of neutrinos
(Boris Kayser)
9
What is the absolute mass scale? How far above
zero is the pattern?
Oscillation data
Cosmological data
10
Do neutrinos have Majorana masses?
Majorana masses for quarks and charged leptons
are forbidden due to charge conservation.
If neutrinos do have Majorana masses then they
must have a very different origin to quark and
charged lepton masses.
11
What are the neutrino dipole moments?
In the SM loop diagrams like this produce a
dipole moment for a Dirac neutrino
A Majorana neutrino cannot have a dipole moment.
12
(No Transcript)
13
Double beta decay
14
(No Transcript)
15
(No Transcript)
16
(No Transcript)
17
(No Transcript)
18
(No Transcript)
19
SNO
20
(No Transcript)
21
(No Transcript)
22
Neutrino oscillation
23
Latest MINOS results (H. Gallagher)
Charged current
Preliminary result arXivhep-ex/0806.2237
24
Preliminary results
25
(No Transcript)
26
Preliminary results
Preliminary result arXivhep-ex/0807.2424
27
Super-K (J. Raaf)
28
(No Transcript)
29
(No Transcript)
30
(No Transcript)
31
3rd and final phase of SNO (R. Robertson)
32
(No Transcript)
33
(No Transcript)
34
(No Transcript)
35
(No Transcript)
36
(No Transcript)
37
(No Transcript)
38
New detector developments
39
Coherent neutrino scattering (J. Collar)
This is a SM process but has yet to be observed.
The cross-section is enhanced if the energy of
the neutrino is less than a few tens of
MeV. Cross-section is proportional to N2. Small
detectors1 kg.
40
Coherent neutrino scattering (J. Collar)
So far this effect has not been observed
41
Megaton Detectors(Andre Rubbia)
42
(No Transcript)
43
(No Transcript)
44
(No Transcript)
45
(No Transcript)
46
(No Transcript)
47
Implications of results from cosmic rays
including the Pierre Auger observatory.(Subir
Sakar and Estaban Roulet)
48
The Pierre Auger Observatory
49
(No Transcript)
50
(No Transcript)
51
The primary particles in the CRs are not photons
Auger found that the
The data from Auger indicates that the main
primary maybe heavy nucleii. These are more
easily accelerated to these extremely high
energies.
52
Heavy neutrinos and geo-neutrinos.
53
Search for heavy neutrinos(Vanucci)
54
PS 191 was used to search for heavy neutrinos.
Not excluded by the MINIBOONE excess
55
(No Transcript)
56
Geo-Neutrinos (Learned McDonough)
Measuring the electron antineutrino flux of the
Earth will improve our models of its structure.
The questions geologists want our help with are
57
(No Transcript)
58
Large scintillator detectors used to detect
antineutrinos from the Earth
59
(No Transcript)