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Discovery of the Neutrino Mass P1X* Frontiers of Physics Lectures 21-22 October 2003 Dr Paul Soler.

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Presentation on theme: "Discovery of the Neutrino Mass P1X* Frontiers of Physics Lectures 21-22 October 2003 Dr Paul Soler."— Presentation transcript:

1 Discovery of the Neutrino Mass P1X* Frontiers of Physics Lectures October 2003 Dr Paul Soler University of Glasgow

2 2 Discovery of the Neutrino Mass Outline 1. Introduction: the structure of matter 2. Neutrinos: 2.1 Neutrino interactions 2.2 Neutrino discovery and questions 2.3 Neutrino oscillations 3. Atmospheric neutrinos 3.1 Superkamiokande experiment 3.2 Discovery of neutrino mass 3.3 Long-baaseline neutrino experiments 4. The Solar Neutrino Puzzle: 4.1 Solar model and the Homestake experiment 4.2 Kamiokande and Superkamiokande experiments 4.3 Gallium experiments 4.4 Sudbury experiment: the solution of the puzzle 5. The future: a neutrino factory?

3 3 Discovery of the Neutrino Mass Motivation Motivation for the Frontiers of Physics lectures: 1.Bring to your attention some of the most exciting fields of physics research at a level that can be easily understood 2.Help you to understand the link between undergraduate physics and front-line research. 3.Use some of the concepts learned in these lectures to improve understanding of undergraduate physics Neutrino physics: exciting recent discoveries have shown that neutrinos have mass, Nobel prizes for R. Davis and M. Koshiba. Motivation for the Discovery of the Neutrino Mass lectures:

4 4 Discovery of the Neutrino Mass References 1.Detecting Massive Neutrinos, E. Kearns, T. Kajita, Y. Totsuka, Scientific American, August Solving the Solar Neutrino Problem, A.B. McDonald, J.R. Klein, D.L. Wark, Scientific American, April Reading for the Discovery of Neutrino Mass lectures Web references: 2002 Nobel Prize in Physics: Super-Kamiokande and K2K web-sites: Sudbury web-site: More on neutrinos:

5 5 Discovery of the Neutrino Mass 1. The structure of matter o How do we find out about the smallest constituents of matter? –Build more powerful microscopes: Wavelength of probe becomes smaller as energy (momentum) of probe becomes larger. For sub-atomic particles, we use powerful accelerators (e.g. CERN, Fermilab).

6 6 Discovery of the Neutrino Mass 1. The structure of matter (cont.) o Two types of particles: –Fermions (half-integer spin particles): make up the known matter and occupy space because of Pauli exclusion principle. Examples: quarks, protons, neutrons, electrons, muons, neutrinos,... –Bosons (integer spin particles): carriers of the forces between fermions Examples: photons for electromagnetic interactions, W and Z bosons for weak interactions, gluons for strong interactions o Fermions come in three families (why?, we dont know) and have antiparticles as well. One neutrino for every electron, muon and tau. Electrons take up space Muons unstable (cosmic rays) Taus very unstable Quarks give most of mass Protons: uud Neutrons: ddu Exotic quarks: rare and unstable

7 7 Discovery of the Neutrino Mass 1. The structure of matter (cont.) o Forces: –Gravity: very weak, long interaction, mediated by graviton (never observed!). –Electromagnetic: keeps atoms together, mediated by photon –Strong: keeps nuclei and nucleons (ie. protons, neutrons) together, mediated by gluons. Very short range interaction –Weak: responsible for some radioactive decays (ie. beta decay), mediated by W +, W - and Z 0 massive gauge bosons. Relatively short range and weak due to mass of the bosons.

8 8 Discovery of the Neutrino Mass 2. Neutrinos: o Neutrinos: –Originally suggested by Pauli in 1930 as a desperate remedy to overcome law of conservation of energy in beta decay: –The neutrino was originally postulated as a massless, chargeless and very weakly interacting particle: practically indetectable! 1.05 KE (MeV ) Radium-E spectrum (Bi-210) Number beta rays Why is the electron spectrum continuous? A third particle (neutrino) is taking away part of the energy

9 9 Discovery of the Neutrino Mass 2.1 Neutrino interactions o Neutrino interactions: –One of the ways neutrinos interact is through inverse beta decay: –Cross-section (average area of neutrino in collision) is very small: on average a neutrino would travel 1600 light-years of water before interacting! light-years or Mean free path: In water:

10 10 Discovery of the Neutrino Mass 2.2 Neutrino discovery o Reines and Cowan observed neutrinos for the first time in 1953 (Nobel prize for Reines in 1995) o They used 400 l of a mixture of water and cadmium chloride (Cd) o An antineutrino from a nuclear reactor (6 x10 20 s -1 ) very rarely interacted with the protons in the target (2.8 hr -1 ): – The positron (e + ) produces two photons, followed about 20 ms later by the neutron interacting with a Cd nucleus that produced another spray of photons Scintillator H 2 O + CdCl 2

11 11 Discovery of the Neutrino Mass 2.2 Neutrino questions Neutrinos are all around us: – Produced by nuclear reactions in radioactive rocks (trace uranium thorium in granite, etc.), in the sun (solar neutrinos) and from cosmic rays hitting the atmosphere (atmospheric neutrinos). – Very difficult to detect because they are so weakly interacting. – Produced in copious quantities inside nuclear reactors. – Generated by high energy accelerators Two main problems: – Solar neutrino problem: nuclear reactions in the sun produce electron neutrinos e (energies up to 14 MeV). The number detected on earth by experiments is between 30%-50% of what is expected. – Atmospheric neutrino problem: high energy particles (cosmic rays) hitting the upper part of the atmosphere. There should be twice as many muon neutrinos as electron neutrinos e (energies up to 10 GeV). Experiments detect approximately equal numbers. Both can be resolved through neutrino oscillations

12 12 Discovery of the Neutrino Mass 2.3 Neutrino oscillations o If neutrinos have mass, theoretically, a neutrino of one species could change into another species: – For example: a muon neutrino changes into a tau neutrino – Probability that a of energy E converts to a after travelling a distance L is: Notice that the probability of oscillations is zero if the mass of the neutrinos are zero! L=length of neutrino path (in m)E=energy neutrino (in MeV) m mass of (in eV)m mass of (in eV) mixing angle between two neutrinos (eV= electronVolt=energy of one electron accelerated by 1 Volt=1.6x J)

13 13 Discovery of the Neutrino Mass 3. Atmospheric Neutrinos o Cosmic rays provide an abundant source of neutrinos. o Protons hit upper part of atmosphere producing cascade of particles including pions that decay (on average) into 2 muon neutrinos for each electron neutrino produced in an interaction

14 14 Discovery of the Neutrino Mass 3.1 Super-Kamiokande experiment o Kamiokande experiment: started 1987, 5000 tons water, 1000 photomultipliers o Super-kamiokande experiment: started 1997 (M. Koshiba leader experiment) 50,000 tons of water, surrounded by 11,000 phototubes to detect flashes of light in the water. Super-Kamiokande experiment is underground Inside a mine in Japan to shield it from the very large number of cosmic rays.

15 15 Discovery of the Neutrino Mass 3.1 Super-Kamiokande experiment o Super-Kamiokande detects faint flashes of Cherenkov light inside huge tank of 50,000 tons of water. o Electron neutrinos make a recoil electron and muon neutrinos make a recoil muon. o Rings of Cherenkov light are formed from the electron or the muon. The detector can distinguish between electrons (fuzzy rings) and muons (clean edge on ring).

16 16 Discovery of the Neutrino Mass 3.2 Discovery of neutrino mass o Results from Super-Kamiokande: – There are less muon neutrinos than expected. The number of muon neutrinos disappearing depends on the angle of the neutrino (ie. It depends on whether the neutrino was produced in the atmosphere above or on the other side of the earth). First evidence for neutrino oscillations in 1998 !!!!

17 17 Discovery of the Neutrino Mass 3.2 Discovery of neutrino mass o As the distance from production increases then more muon neutrinos disappear. Therefore 84% of survive journey!

18 18 Discovery of the Neutrino Mass 3.2 Discovery of neutrino mass Consequences of discovery: – Neutrino oscillations responsible for atmospheric muon neutrino deficit. – Since electron neutrino spectrum well predicted, it must be muon neutrinos changing into tau neutrinos. – Since then neutrinos have mass!! – Mass of the neutrinos have to be greater than eV. If either the or is much smaller than the other, then m ~0.05 eV. Both or could have a mass much larger than m ~0.05 eV as long as the difference of the mass squared is 3.2x10 -3 eV 2. Since there were so many neutrinos produced soon after the big- bang, if they have a mass, it could provide a large portion of the missing mass of the universe (up to 20%).

19 19 Discovery of the Neutrino Mass 3.3 Long-baseline experiments Long-baseline experiments with accelerators will verify that oscillations are really taking place in Super-Kamiokande. – K2K (from the KEK accelerator in Japan to Super-Kamiokande): 250 km baseline of neutrinos. So far they observe 56 events when they expected 80 events, consistent with 3x10 -3 eV 2 mass-squared difference. – MINOS: neutrino beam from Fermilab in Chicago to a mine in Minnesotta (750 km), will start taking data in Another beam from CERN to Gran Sasso (CNGS) laboratory in Italy (also 750 km) to start in 2006.

20 20 Discovery of the Neutrino Mass 4. Solar Neutrinos

21 21 Discovery of the Neutrino Mass 4. The Solar Neutrino Puzzle o Ray Davis (Brookhaven National Laboratory) proposed an experiment in the 1960s to measure neutrinos from the sun. o Why are neutrinos emitted from the sun? o Nuclear fusion powers sun: o Energy of sun is due to burning hydrogen into helium. The measured photon luminosity is: 3.9x10 26 J s -1. Energy per neutrino = 26.7x10 6 x1.6x = 4.3x J/neutrino Number of neutrinos = 3.9x10 26 /4.3x = 9.1x10 37 neutrino s -1 Distance from sun to earth =R= 1.5x10 13 cm. Therefore: (64 billion neutrinos per second through your finger nail of 1 cm 2 !!!!)

22 22 Discovery of the Neutrino Mass 4. The Solar Model o In reality, chain of reactions needed to burn 4 hydrogen nuclei into helium nucleus. o There are two main cycles: the pp cycle (98.5% of the total suns power comes from these reactions) and the CNO cycle catalysed by carbon, nitrogen and oxygen (not very important in the sun with only 1.5% of power output). o Most abundant neutrinos are low energy (<0.42 MeV) pp reaction with flux 6.0x10 10 cm -2 s -1. Most important for detection are 8 B neutrinos because they have high energy (<14 MeV) but only consist of of all solar neutrinos. PP cycle:

23 23 Discovery of the Neutrino Mass 4.1 Homestake experiment o Ray Davis Chlorine experiment inside Homestake mine in Lead, South Dakota: 100,000 gallons (615 tons) of cleaning fluid (C 2 Cl 4 ) Expect about 1.5 Ar atoms/day

24 24 Discovery of the Neutrino Mass 4.1 Homestake and Solar Model o Results from the Ray Davis chlorine experiment: sensitive to 8 B and 7 Be neutrinos (0.814 MeV threshold). Measured SNU (0.48 atoms/day), Solar Model Expectation = SNU (1.5 atoms/day) Observation about 1/3 the expected number of solar neutrinos 1 SNU = 1 interaction per target atoms per second Is there something wrong with experiment, something wrong with solar model or something wrong with the neutrinos?

25 25 Discovery of the Neutrino Mass 4.2 Super-Kamiokande experiment o Results Super-Kamiokande experiment: can also measure solar neutrinos –Proof that neutrinos come from sun: angular correlation –Neutrino flux is 46.5% that expected from the solar model Confirmation Solar Neutrino Puzzle!

26 26 Discovery of the Neutrino Mass 4.3 Gallium experiments o Similar experiments to chlorine but with gallium: –Lower threshold (0.233 MeV) so sensitive to the lower end of the pp chain –Further evidence of missing solar neutrinos (55% of expectation) Expectation: SNU Observed: SNU

27 27 Discovery of the Neutrino Mass 4.4 Sudbury Neutrino Observatory o Heavy water (D 2 O) experiment in Canada: 1000 tonnes D 2 O Acrylic Vessel PMTs Phototube Support Structure (PSUP) 6500 tonnes H 2 O Surface: 2 km (D=deuterium= proton+neutron)

28 28 Discovery of the Neutrino Mass 4.4 Sudbury Neutrino Observatory o Acryllic vessel with photomultiplier tubes: All components Made out of very low radioactivity materials

29 29 Discovery of the Neutrino Mass 4.4 Sudbury Neutrino Observatory o Faint flashes of Cherenkov light recorded by photomultipliers:

30 30 Discovery of the Neutrino Mass 4.4 Sudbury Neutrino Observatory o Results: –Charged current (CC): –Elastic scattering (ES): –Neutral current (NC): CC ES NC #EVENTS About 35% electron neutrinos make it to earth (from CC) but flux of all neutrino species (from NC and ES) as expected: Neutrinos change species in flight: (35% SSM) (100% SSM) Neutrino Oscillations!

31 31 Discovery of the Neutrino Mass 4.4 Solar neutrino puzzle solution o Sudbury Neutrino Observatory has confirmed neutrino oscillations from solar neutrinos and has confirmed the solar model of fusion in the sun. Experiments only sensitive to electron neutrinos ( e ) see a deficit but Sudbury experiment that is sensitive to all neutrino flavours sees the expected total number of neutrinos. Electron neutrinos ( e ) oscillated into muon neutrinos ( ) in trajectory from the sun to the earth. However, the evidence shows that the transition happened inside the sun, due to an enhancement of the oscillations because of the high matter density of the sun. o Parameters:

32 32 Discovery of the Neutrino Mass 4.4 Solar neutrino puzzle solution o More confirmation: KamLAND experiment in Kamioka mine in Japan shows that reactor (~2 MeV) disappearing in flight (~180 km).

33 33 Discovery of the Neutrino Mass 4.5 The future: a neutrino factory? o Future directions for neutrino physics: build a neutrino factory to fire very intense beams of neutrinos at 700 km to one experiment and around 7000 km to other side of the world. o Main aim: why is the universe made of matter rather than antimatter? CP violation of neutrino oscillations might be explanation and a neutrino factory could measure this effect.

34 34 Discovery of the Neutrino Mass Conclusions o Neutrinos are very misterious particles and we are only starting to undertand their nature. Super-Kamiokande experiment discovered neutrino oscillations ( to from the deficit of muon neutrinos from cosmic rays hitting the upper layers of the atmosphere. This implies that neutrinos have mass with mass- squared difference of 3x10 -3 eV 2 (largest mass greater than 0.05 eV). A number of experiments looking at solar neutrinos have also seen a deficit in the number of electron neutrinos from the sun. Confirmation of neutrino oscillations in solar neutrinos came from the Sudbury experiment that showed that it is only the electron neutrinos that are missing while the total flux of neutrinos is as expected. Hence electron neutrinos e are changing to another species (probably with a mass-squared difference of 7.1x10 -5 eV 2. o The field of neutrino physics still has a bright future, with open questions: –What is the absolute mass of neutrinos? –Are neutrinos their own antiparticle? –And the most ambitious question of all: are neutrinos responsible for the matter-antimatter asymmetry of the universe?

35 35 Discovery of the Neutrino Mass


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