University of Puerto Rico at Mayagüez NEUTRINO PHYSICS SEMINAR Speaker: Marvin Santos Graduate Seminar I Advisor: Héctor Méndez Physics Department At the subatomic level, our world is made up of different particles. There is one type of particle, however, that passes by without attracting any attention to itself. A neutrino has a tiny mass and carries no electrical charge. Therefore, it doesn't feel the electromagnetic force, that dominates at atomic scales, and will pass through most matter with no effect. This creates an almost undetectable particle, despite the fact trillions pass through the Earth every second. Why are neutrinos important? The discovery a couple of years ago that neutrinos have mass, contrary to what was previously thought, has revolutionized our understanding of neutrinos while raising new questions about matter, energy, space and time. Neutrinos may play a key Origen of Unification role in solving the mystery of how the universe came to consist of matter rather than antimatter. They Matter Forces could also unveil new, exotic physical processes that have been far beyond our reach.
Beta Decay Black Hole Formation
Date: Tuesday, October 23 /2018 @ 4:30 pm Place: Physics Building, Classroom F-461 Neutrino Physics Seminar
Marvin Santos
Graduate Seminar I Advisor: Héctor Méndez, Ph.D Physics Deparment University of Puerto Rico at Mayagüez PR-108, Mayagüez, 00682 Puerto Rico
August 23, 2018
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 1 / 43 Table of Contents
K 0 1 Standard Model Invariant Mass of the s 6 List of Neutrino Experiments 2 Introduction to Neutrinos Famous Neutrino Observatories 3 History Deep Underground Neutrino Experiment Pauli’s Proposal Super-Kamiokande Direct Detection IceCube Neutrino Observatory Neutrino Flavor 7 Applications Solar Neutrino Problem Faster Global Communications Oscillation First Message Using Neutrino Beam 4 Neutrino Research Extraterrestrial Communications Cosmic Neutrinos 8 Videos 5 Proton Decay 9 Conclusions Some Channels of Proton Decay 10 References
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 2 / 43 Standard Model Standard Model
The Standard Model of particle physics is the theory describing three of the four known fundamental forces (the electromagnetic, weak, and strong interactions, and not including the gravitational force) in the universe, as well as classifying all known elementary particles. It was developed in stages throughout the latter half of the 20th century, through the work of many scientists around the world.
Figure: Modelo Estándar Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 3 / 43 Introduction to Neutrinos Introduction to Neutrinos
A neutrino (denoted by the Greek letter ν) is a fermion (an elementary particle with half-integer spin) that interacts only via the weak subatomic force and gravity. The mass of the neutrino is much smaller than that of the other known elementary particles. [2]
Figure: The first use of a hydrogen bubble chamber to detect neutrinos, on 13 November 1970, at Argonne National Laboratory.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 4 / 43 Introduction to Neutrinos How many neutrinos are passing through us?
The number of solar neutrinos that reach us on the earth is measured by something called “flux”, which is how science geeks measure the rate of flow of material. The solar neutrino flux for us on Earth is about 65 billion neutrinos, passing through just one square centimeter of area on earth, every second.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 5 / 43 Introduction to Neutrinos Neutrino Flux from the Sun
Overall result of the proton-proton (p-p) chain of reactions:
4 + 4 × p →2 He + 2e 2νe (1) 28 MeV of energy shared between the reaction products and note that this reaction conserves:Charge (+4), Baryon number (4), Lepton number (0). Luminosity of the sun is 3.9 × 1033 erg/s
nreaction/s × Ereaction = Lsun nreaction/s × 2neutrinos/reaction Fneutrinos = Lsun Area nreaction/s = Ereaction Lsun 1 2 Fneutrinos = × 2 × 2 neutrinos/s · cm Lsun Ereaction 4πd nreaction/s = 2 10 2 mc Fneutrinos = 6.5 × 10 neutrinos/s · cm
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 6 / 43 History Pauli’s Proposal Pauli’s Proposal
The neutrino was postulated first by Wolfgang Pauli in 1930 to explain how beta decay could conserve energy, momentum, and angular momentum (spin). In contrast to Niels Bohr, who proposed a statistical version of the conservation laws to explain the observed continuous energy spectra in beta decay.
Figure: Beta Decay
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 7 / 43 History Pauli’s Proposal Fermi’s Interaction
In particle physics, Fermi’s interaction (also the Fermi theory of beta decay) is an explanation of the beta decay, proposed by Enrico Fermi in 1933. This interaction explains beta decay of a neutron by direct coupling of a neutron with an electron, a neutrino (later determined to be an antineutrino) and a proton.
Figure: Beta Decay
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 8 / 43 History Direct Detection Direct Detection
In 1942, Wang Ganchang first proposed the use of beta capture to experimentally detect neutrinos.[4] In the 20 July 1956 issue of Science, Clyde Cowan, Frederick Reines, F. B. Harrison, H. W. Kruse, and A. D. McGuire published confirmation that they had detected the neutrino, a result that was rewarded almost forty years later with the 1995 Nobel Prize.
Figure: Clyde Cowan conducting the neutrino experiment circa 1956
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 9 / 43 History Neutrino Flavor Neutrino Flavor
The antineutrino discovered by Cowan and Reines is the antiparticle of the electron neutrino. In 1962, Leon M. Lederman, Melvin Schwartz and Jack Steinberger showed that more than one type of neutrino exists by first detecting interactions of the muon neutrino (already hypothesised with the name neutretto),[25] which earned them the 1988 Nobel Prize in Physics.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 10 / 43 History Solar Neutrino Problem Solar Neutrino Problem
In the 1960s, the now-famous Homestake experiment made the first measurement of the flux of electron neutrinos arriving from the core of the Sun and found a value that was between one third and one half the number predicted by the Standard Solar Model. This discrepancy, which became known as the solar neutrino problem, remained unresolved for some thirty years, while possible problems with both the experiment and the solar model were investigated, but none could be found.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 11 / 43 History Solar Neutrino Problem Solar Neutrinos
Solar neutrinos (proton–proton chain) in the Standard Solar Model.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 12 / 43 History Oscillation Oscillation
Neutrino oscillation is a quantum mechanical phenomenon whereby a neutrino created with a specific lepton family number ("lepton flavor": electron, muon, or tau) can later be measured to have a different lepton family number. The probability of measuring a particular flavor for a neutrino varies between 3 known states, as it propagates through space. The states with a flavor are not states with a certain mass, but rather an overlap of the possible masses:
|νei = 0.8 |ν1i + 0.5 |ν2i ± 0.2 |ν3i
|νµi = 0.4 |ν1i − 0.5 |ν2i + 0.7 |ν3i
|ντ i = −0.4 |ν1i + 0.6 |ν2i + 0.7 |ν3i
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 13 / 43 History Oscillation The matter-antimatter asymmetry problem
The Big Bang should have created equal amounts of matter and antimatter in the early universe. But today, everything we see from the smallest life forms on Earth to the largest stellar objects is made almost entirely of matter. Comparatively, there is not much antimatter to be found.
Oscillations that could herald an answer to one of the biggest mysteries in physics: why matter dominates over antimatter in the universe. Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 14 / 43 Neutrino Research Neutrino Research
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 15 / 43 Neutrino Research Cosmic Neutrinos Cosmic Neutrinos
Raymond Davis, Jr. and Masatoshi Koshiba were jointly awarded the 2002 Nobel Prize in Physics. Both conducted pioneering work on solar neutrino detection, and Koshiba’s work also resulted in the first real-time observation of neutrinos from the SN 1987A supernova in the nearby Large Magellanic Cloud. These efforts marked the beginning of neutrino astronomy.[3]
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 16 / 43 Proton Decay Proton Decay
In particle physics, proton decay is a hypothetical form of particle decay in which the proton decays into lighter subatomic, as a neutral pion and a positron on antineutrino and kaon positive (golden mode or most likely mode) For the decay p → ν¯K + it would have that the baryonic numbers are:
p → ν K +
B : 1 0 0 B : 1 =6 0 + 0 For the decay p → e Ks it would have that the baryonic numbers are:
+ 0 p → e Ks
B : 1 0 0 B : 1 =6 0
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 17 / 43 Proton Decay Some Channels of Proton Decay Proton Decay
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 18 / 43 Proton Decay Some Channels of Proton Decay Proton Decay
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 19 / 43
+ 0 Figure: Topología del canal p → e Ks Proton Decay Some Channels of Proton Decay Some Channels of Proton Decay
After some tests with some channels the study will be emphasized to the channel
+ 0 p → e Ks
0 Where the Ks decays in turn to: 0 + − Ks → π π 0 since for our study, there are more possibilities to reconstruct the invariant mass of the Ks .
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 20 / 43 0 Proton Decay Invariant Mass of the Ks 0 Invariant Mass of the Ks
0 + 0 Masa invariante Ks corte 3, p -> e ks reco
20
18
16 /canal/eventos 2 14
12 20 MeV/c 10
8
6
4
2
0 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1 Masa invariante (GeV/c2)
0 + 0 Figure: Distribution of invariant mass for candidates to Ks (canal p → e Ks ).
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 21 / 43 List of Neutrino Experiments Neutrino detectors, experiments, and facilities
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 22 / 43 List of Neutrino Experiments Famous Neutrino Observatories Famous Neutrino Observatories
1 The Deep Underground Neutrino Experiment (DUNE). 2 Super-Kamiokande. 3 Icecube Neutrino Observatory.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 23 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment Deep Underground Neutrino Experiment
DUNE is a leading-edge, international experiment for neutrino science and proton decay studies. Discoveries over the past half-century have put neutrinos, the most abundant matter particles in the universe, in the spotlight for further research into several fundamental questions about the nature of matter and the evolution of the universe — questions that DUNE will seek to answer.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 24 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 25 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment Building an International Flagship Neutrino Experiment
An international team of over 1,000 scientists and engineers from more than 30 countries are building the most advanced neutrino experiment in the world, which could change our understanding of the universe. Groundbreaking for this revolutionary endeavor—hosted by the U.S. Department of Energy’s Fermilab with contributions from across the U.S. and around the globe—took place in July of 2017.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 26 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 27 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment Production of a Neutrino Beam
Figure: A diagram of the design and production of a neutrino beam
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 28 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment
Figure: Location of detectors in LBNF
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 29 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment Argon
The detector is planned to consist of four separate modules, of two different designs, to be installed in two long caverns. Groundbreaking for the excavation of the caverns took place in July 2017. The detector modules will hold a combined total of 68,000 tons of liquid argon (LAr), which is the target material for neutrino interactions. Argon, a gas at room temperature, condenses to a liquid when cooled below -186°C (-303°F) and requires containment in well insulated cryostats and a sophisticated cooling infrastructure.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 30 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment
Figure: The DUNE far detector will comprise four cryogenic modules, each of which will hold 17,000 tons of liquid argon. A central utility cavern will house the cryogenics system as well as electrical power equipment, air-handling units, and other support equipment.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 31 / 43 List of Neutrino Experiments Deep Underground Neutrino Experiment Cross Section of the Far Detector
Figure: Cross section of the Far detector of 17kT
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 32 / 43 List of Neutrino Experiments Super-Kamiokande Super-Kamiokande
The Super-Kamiokande experiment – located a kilometre underground in central Japan -consists of a tank filled with 50 000 tons of water surrounded by photomultiplier tubes. These tubes detect the faint flashes of light known as Cerenkov radiation given off by electron - and muon-neutrinos when they interact with electrons in the water molecules.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 33 / 43 List of Neutrino Experiments Super-Kamiokande Cherenkov radiation
Speed of light in a medium (e.g. water) is less than the speed of light in vacuum - therefore possible for an energetic particle to move at v > speed of light.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 34 / 43 List of Neutrino Experiments Super-Kamiokande Sun in Neutrino
Sun in neutrino light, as seen by the SuperKamiokande.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 35 / 43 List of Neutrino Experiments Super-Kamiokande The Cosmic Neutrino Background CνB
The CνB[1] is a relic of the big bang; while the cosmic microwave background radiation (CMB) dates from when the universe was 379,000 years old, the CνB decoupled (separated) from matter when the universe was just one second old.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 36 / 43 List of Neutrino Experiments IceCube Neutrino Observatory IceCube Neutrino Observatory
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 37 / 43 Applications Faster Global Communications Faster Global Communications
1 Drawback of Electromagnetic wave is they don’t passes through all matter. 2 Neutrinos easily penetrate through all matter. 3 With almost the speed of light. 4 Communication tool for future.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 38 / 43 Applications First Message Using Neutrino Beam First Message Using Neutrino Beam
1 On Apr 2012, scientists of Fermilab send a first message using neutrino beam. 2 They convert Neutrino to binary code. 3 Distance over 1035 m with 240 m of Earth. 4 Successfully received by MINERvA detector.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 39 / 43 Applications Extraterrestrial Communications Extraterrestrial Communications
1 Neutrinos plays a great role in SETI. 2 Penetrate massive interstellar clouds. 3 Detection neutrino carrying information provide evidence of Alien civilizations.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 40 / 43 Videos Videos
The Science of the Deep Underground Neutrino Experiment (DUNE)
Small Particles, Big Science: The International LBNF/DUNE Projec
Prototype detectors for the Deep Underground Neutrino Experiment
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 41 / 43 Conclusions Conclusions
1 Neutrinos have the secret of the Universe. 2 Neutrino have a power to solve the unsolved mysteries of Science. 3 The mass of neutrinos has such a small value
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 42 / 43 References References
Brent Follin, Lloyd Knox, Marius Millea, and Zhen Pan. First detection of the acoustic oscillation phase shift expected from the cosmic neutrino background. Phys. Rev. Lett., 115:091301, Aug 2015. Susanne Mertens. Direct neutrino mass experiments. Journal of Physics: Conference Series, 718(2):022013, 2016. G. Pagliaroli, F. Vissani, M.L. Costantini, and A. Ianni. Improved analysis of sn1987a antineutrino events. Astroparticle Physics, 31(3):163 – 176, 2009. Kan Chang Wang. A suggestion on the detection of the neutrino. Phys. Rev., 61:97–97, Jan 1942.
Marvin Santos (UPRM) Neutrino Physics Seminar August 23, 2018 43 / 43