Relic Supernova νʻs. Stanley Wojcicki
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1 Relic Supernova νʻs 53
2 Relic Supernova νʻs In the whole universe, supernovas occur very frequently They leave behind relic neutrinos 53
3 Relic Supernova νʻs In the whole universe, supernovas occur very frequently They leave behind relic neutrinos Difficult to detect in water Cerenkov counters; due to backgrounds from reactor and atmospheric νʻs 53
4 Relic Supernova νʻs In the whole universe, supernovas occur very frequently They leave behind relic neutrinos Difficult to detect in water Cerenkov counters; due to backgrounds from reactor and atmospheric νʻs SuperK limit 53
5 Relic Supernova νʻs In the whole universe, supernovas occur very frequently They leave behind relic neutrinos Difficult to detect in water Cerenkov counters; due to backgrounds from reactor and atmospheric νʻs SuperK limit Possibility: dissolve Gd in water; use double coincidence for νʻs 53
6 Relic Supernova νʻs In the whole universe, supernovas occur very frequently They leave behind relic neutrinos Difficult to detect in water Cerenkov counters; due to backgrounds from reactor and atmospheric νʻs SuperK limit Applications: SuperK HyperK DUSEL Possibility: dissolve Gd in water; use double coincidence for νʻs 53
7 Searches for UHE νʻs 54
8 Searches for UHE νʻs High Energy νʼs must be present because of GZK mechanism p + γ CMB Δ + π + + n π + µ + + ν µ µ + e + + ν e + ν µ 54
9 Searches for UHE νʻs High Energy νʼs must be present because of GZK mechanism p + γ CMB Δ + π + + n π + µ + + ν µ µ + e + + ν e + ν µ here a number of potential high energy ν sources (AGNʼs, GRBʼs, etc) whose observation would be exciting 54
10 Searches for UHE νʻs High Energy νʼs must be present because of GZK mechanism p + γ CMB Δ + π + + n π + µ + + ν µ µ + e + + ν e + ν µ here a number of potential high energy ν sources (AGNʼs, GRBʼs, etc) whose observation would be exciting Various efforts: IceCube (Antarctica Ice), ANTARES (under water), Auger (fluorescence, large shower array), ANITA (balloons, radio waves) No positive results yet but current limits are getting close to predictions in some models 54
11 Searches for UHE νʻs High Energy νʼs must be present because of GZK mechanism p + γ CMB Δ + π + + n π + µ + + ν µ µ + e + + ν e + ν µ here a number of potential high energy ν sources (AGNʼs, GRBʼs, etc) whose observation would be exciting Various efforts: IceCube (Antarctica Ice), ANTARES (under water), Auger (fluorescence, large shower array), ANITA (balloons, radio waves) No positive results yet but current limits are getting close to predictions in some models Note: Earth stops being transparent to νʼs around ev 54
12 Neutrinos at the LHC 55
13 Ideas re ν mass? 56
14 Ideas re ν mass? Favorite view: νʻs are Majorana particles; their mass is generated by some seesaw mechanism 56
15 Ideas re ν mass? Favorite view: νʻs are Majorana particles; their mass is generated by some seesaw mechanism In brief: the mass of the observed (light) νʻs is inversely related to some higher mass scale: m = Y v2 ν M ν L NR 56
16 Ideas re ν mass? Favorite view: νʻs are Majorana particles; their mass is generated by some seesaw mechanism In brief: the mass of the observed (light) νʻs is inversely related to some higher mass scale: m = Y v2 ν M ν L NR In the original form, Y (Yukawa coupling) ~1, M is the mass of heavy right handed neutrino (related to the GUT scale) and v is typical electro weak mass 56
17 Ideas re ν mass? Favorite view: νʻs are Majorana particles; their mass is generated by some seesaw mechanism In brief: the mass of the observed (light) νʻs is inversely related to some higher mass scale: m = Y v2 ν M ν L NR In the original form, Y (Yukawa coupling) ~1, M is the mass of heavy right handed neutrino (related to the GUT scale) and v is typical electro weak mass 56
18 Other possibilities Recently a lot of theoretical interest in exploring other models within this general scenario but with the high mass scale ~TeV, ie observable at the LHC Extended seesaw models have, instead of heavy new scalar, heavy scalar triplet (Type II seesaw) or heavy fermion triplet (Type III) These could be produced at the LHC if in the TeV mass range 57
19 Other possibilities Recently a lot of theoretical interest in exploring other models within this general scenario but with the high mass scale ~TeV, ie observable at the LHC Extended seesaw models have, instead of heavy new scalar, heavy scalar triplet (Type II seesaw) or heavy fermion triplet (Type III) These could be produced at the LHC if in the TeV mass range The signature would be observation of 2 like sign leptons 57
20 Practical Applications? ν 's $,, 58
21 Few Typical Ideas 59
22 Few Typical Ideas Are neutrinos too esoteric to be practical? Several ideas have been put forth in the past 59
23 Few Typical Ideas Are neutrinos too esoteric to be practical? Several ideas have been put forth in the past a) Remote monitoring of nuclear reactors Probably most practical of different suggestions 59
24 Few Typical Ideas Are neutrinos too esoteric to be practical? Several ideas have been put forth in the past a) Remote monitoring of nuclear reactors Probably most practical of different suggestions b) Communications Interstellar communications Deep sea communications with submarines 59
25 Few Typical Ideas Are neutrinos too esoteric to be practical? Several ideas have been put forth in the past a) Remote monitoring of nuclear reactors Probably most practical of different suggestions b) Communications Interstellar communications Deep sea communications with submarines c) Tomography of the earth, geological explorations eg A.DeRujula, S.Glashow, R.R.Wilson and G.Charpak (1983) 59
26 νʻs and Other Sciences 60
27 νʻs and Other Sciences Impact on Cosmology, Astrophysics, Astronomy Supernova Mechanisms Early Supernova Warning Solar Models Beyond GZK energy region 60
28 νʻs and Other Sciences Impact on Cosmology, Astrophysics, Astronomy Supernova Mechanisms Early Supernova Warning Solar Models Beyond GZK energy region Connection with Geophysics Chemical composition of the mantle 60
29 νʻs and Other Sciences Impact on Cosmology, Astrophysics, Astronomy Supernova Mechanisms Early Supernova Warning Solar Models Beyond GZK energy region Connection with Geophysics Chemical composition of the mantle 60
30 Summary and Whatʼs Ahead in the Future people often overestimate what will happen in the next two years and underestimate what will happen in ten - Bill Gates 61
31 The Big Questions 62
32 The Big Questions What is the value of θ13? 62
33 The Big Questions What is the value of θ13? How close to 45 o is θ23? 62
34 The Big Questions What is the value of θ13? How close to 45 o is θ23? What is the value of δcp? 62
35 The Big Questions What is the value of θ13? How close to 45 o is θ23? What is the value of δcp? What is the mass hierarchy? 62
36 The Big Questions What is the value of θ13? How close to 45 o is θ23? What is the value of δcp? What is the mass hierarchy? What is the mass of the lightest ν? 62
37 The Big Questions What is the value of θ13? How close to 45 o is θ23? What is the value of δcp? What is the mass hierarchy? What is the mass of the lightest ν? Are neutrinos Dirac or Majorana? 62
38 The Big Questions What is the value of θ13? How close to 45 o is θ23? What is the value of δcp? What is the mass hierarchy? What is the mass of the lightest ν? Are neutrinos Dirac or Majorana? Are there light sterile neutrinos? 62
39 The Big Questions What is the value of θ13? How close to 45 o is θ23? What is the value of δcp? What is the mass hierarchy? What is the mass of the lightest ν? Are neutrinos Dirac or Majorana? Are there light sterile neutrinos? Is there a heavy NR? How heavy? 62
40 And Some More 63
41 And Some More Are there anomalous ν interactions? 63
42 And Some More Are there anomalous ν interactions? Do νʻs have anomalous electromagnetic properties? 63
43 And Some More Are there anomalous ν interactions? Do νʻs have anomalous electromagnetic properties? Are there new ν phenomena in supernovas? 63
44 And Some More Are there anomalous ν interactions? Do νʻs have anomalous electromagnetic properties? Are there new ν phenomena in supernovas? Why differences (and similarities) between quarks and leptons? 63
45 And Some More Are there anomalous ν interactions? Do νʻs have anomalous electromagnetic properties? Are there new ν phenomena in supernovas? Why differences (and similarities) between quarks and leptons? What is the significance of tri-bimaximal(?) PMNS matrix? 63
46 And Some More Are there anomalous ν interactions? Do νʻs have anomalous electromagnetic properties? Are there new ν phenomena in supernovas? Why differences (and similarities) between quarks and leptons? What is the significance of tri-bimaximal(?) PMNS matrix? What is Dark Matter? 63
47 And Some More Are there anomalous ν interactions? Do νʻs have anomalous electromagnetic properties? Are there new ν phenomena in supernovas? Why differences (and similarities) between quarks and leptons? What is the significance of tri-bimaximal(?) PMNS matrix? What is Dark Matter? Do protons decay? 63
48 And Some More Are there anomalous ν interactions? Do νʻs have anomalous electromagnetic properties? Are there new ν phenomena in supernovas? Why differences (and similarities) between quarks and leptons? What is the significance of tri-bimaximal(?) PMNS matrix? What is Dark Matter? Do protons decay? Do we owe our existence to leptogenesis? 63
49 Future Reactor Expts 64
50 Future Reactor Expts The Challenge ND FD 64
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