13. CP Violation in the Quark Sector
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Estimation of Baryon Asymmetry of the Universe from Neutrino Physics
ESTIMATION OF BARYON ASYMMETRY OF THE UNIVERSE FROM NEUTRINO PHYSICS Manorama Bora Department of Physics Gauhati University This thesis is submitted to Gauhati University as requirement for the degree of Doctor of Philosophy Faculty of Science March 2018 I would like to dedicate this thesis to my parents . Abstract The discovery of neutrino masses and mixing in neutrino oscillation experiments in 1998 has greatly increased the interest in a mechanism of baryogenesis through leptogenesis, a model of baryogenesis which is a cosmological consequence. The most popular way to explain why neutrinos are massive but at the same time much lighter than all other fermions, is the see-saw mechanism. Thus, leptogenesis realises a highly non-trivial link between two completely independent experimental observations: the absence of antimatter in the observable universe and the observation of neutrino mixings and masses. Therefore, leptogenesis has a built-in double sided nature.. The discovery of Higgs boson of mass 125GeV having properties consistent with the SM, further supports the leptogenesis mechanism. In this thesis we present a brief sketch on the phenomenological status of Standard Model (SM) and its extension to GUT with or without SUSY. Then we review on neutrino oscillation and its implication with latest experiments. We discuss baryogenesis via leptogenesis through the decay of heavy Majorana neutrinos. We also discuss formulation of thermal leptogenesis. At last we try to explore the possibilities for the discrimination of the six kinds of Quasi- degenerate neutrino(QDN)mass models in the light of baryogenesis via leptogenesis. We have seen that all the six QDN mass models are relevant in the context of flavoured leptogenesis. -
Baryogenesis and Dark Matter from B Mesons: B-Mesogenesis
Baryogenesis and Dark Matter from B Mesons: B-Mesogenesis Miguel Escudero Abenza [email protected] arXiv:1810.00880, PRD 99, 035031 (2019) with: Gilly Elor & Ann Nelson Based on: arXiv:2101.XXXXX with: Gonzalo Alonso-Álvarez & Gilly Elor New Trends in Dark Matter 09-12-2020 The Universe Baryonic Matter 5% 26% Dark Matter 69% Dark Energy Planck 2018 1807.06209 Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !2 Theoretical Understanding? Motivating Question: What fraction of the Energy Density of the Universe comes from Physics Beyond the Standard Model? 99.85%! Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !3 SM Prediction: Neutrinos 40% 60% Photons Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !4 The Universe Baryonic Matter 5% 26% Dark Matter 69% Dark Energy Planck 2018 1807.06209 Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !5 Baryogenesis and Dark Matter from B Mesons: B-Mesogenesis arXiv:1810.00880 Elor, Escudero & Nelson 1) Baryogenesis and Dark Matter are linked 2) Baryon asymmetry directly related to B-Meson observables 3) Leads to unique collider signatures 4) Fully testable at current collider experiments Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !6 Outline 1) B-Mesogenesis 1) C/CP violation 2) Out of equilibrium 3) Baryon number violation? 2) A Minimal Model & Cosmology 3) Implications for Collider Experiments 4) Dark Matter Phenomenology 5) Summary and Outlook Miguel Escudero (TUM) B-Mesogenesis New Trends in DM 09-12-20 !7 Baryogenesis -
Peering Into the Universe and Its Ele Mentary
A gigantic detector to explore elementary particle unification theories and the mysteries of the Universe’s evolution Peering into the Universe and its ele mentary particles from underground Ultrasensitive Photodetectors The planned Hyper-Kamiokande detector will consist of an Unified Theory and explain the evolution of the Universe order of magnitude larger tank than the predecessor, Super- through the investigation of proton decay, CP violation (the We have been developing the world’s largest photosensors, which exhibit a photodetection Kamiokande, and will be equipped with ultra high sensitivity difference between neutrinos and antineutrinos), and the efficiency two times greater than that of the photosensors. The Hyper-Kamiokande detector is both a observation of neutrinos from supernova explosions. The Super-Kamiokande photosensors. These new “microscope,” used to observe elementary particles, and a Hyper-Kamiokande experiment is an international research photosensors are able to perform light intensity “telescope”, used to study the Sun and supernovas through project aiming to become operational in the second half of and timing measurements with a much higher neutrinos. Hyper-Kamiokande aims to elucidate the Grand the 2020s. precision. The new Large-Aperture High-Sensitivity Hybrid Photodetector (left), the new Large-Aperture High-Sensitivity Photomultiplier Tube (right). The bottom photographs show the electron multiplication component. A megaton water tank The huge Hyper-Kamiokande tank will be used in order to obtain in only 10 years an amount of data corresponding to 100 years of data collection time using Super-Kamiokande. This Experimental Technique allows the observation of previously unrevealed The photosensors on the tank wall detect the very weak Cherenkov rare phenomena and small values of CP light emitted along its direction of travel by a charged particle violation. -
The Matter – Antimatter Asymmetry of the Universe and Baryogenesis
The matter – antimatter asymmetry of the universe and baryogenesis Andrew Long Lecture for KICP Cosmology Class Feb 16, 2017 Baryogenesis Reviews in General • Kolb & Wolfram’s Baryon Number Genera.on in the Early Universe (1979) • Rio5o's Theories of Baryogenesis [hep-ph/9807454]} (emphasis on GUT-BG and EW-BG) • Rio5o & Trodden's Recent Progress in Baryogenesis [hep-ph/9901362] (touches on EWBG, GUTBG, and ADBG) • Dine & Kusenko The Origin of the Ma?er-An.ma?er Asymmetry [hep-ph/ 0303065] (emphasis on Affleck-Dine BG) • Cline's Baryogenesis [hep-ph/0609145] (emphasis on EW-BG; cartoons!) Leptogenesis Reviews • Buchmuller, Di Bari, & Plumacher’s Leptogenesis for PeDestrians, [hep-ph/ 0401240] • Buchmulcer, Peccei, & Yanagida's Leptogenesis as the Origin of Ma?er, [hep-ph/ 0502169] Electroweak Baryogenesis Reviews • Cohen, Kaplan, & Nelson's Progress in Electroweak Baryogenesis, [hep-ph/ 9302210] • Trodden's Electroweak Baryogenesis, [hep-ph/9803479] • Petropoulos's Baryogenesis at the Electroweak Phase Transi.on, [hep-ph/ 0304275] • Morrissey & Ramsey-Musolf Electroweak Baryogenesis, [hep-ph/1206.2942] • Konstandin's Quantum Transport anD Electroweak Baryogenesis, [hep-ph/ 1302.6713] Constituents of the Universe formaon of large scale structure (galaxy clusters) stars, planets, dust, people late ame accelerated expansion Image stolen from the Planck website What does “ordinary matter” refer to? Let’s break it down to elementary particles & compare number densities … electron equal, universe is neutral proton x10 billion 3⇣(3) 3 3 n =3 T 168 cm− neutron x7 ⌫ ⇥ 4⇡2 ⌫ ' matter neutrinos photon positron =0 2⇣(3) 3 3 n = T 413 cm− γ ⇡2 CMB ' anti-proton =0 3⇣(3) 3 3 anti-neutron =0 n =3 T 168 cm− ⌫¯ ⇥ 4⇡2 ⌫ ' anti-neutrinos antimatter What is antimatter? First predicted by Dirac (1928). -
Baryogenesis and Dark Matter from B Mesons
Baryogenesis and Dark Matter from B mesons Abstract: In [1] a new mechanism to simultaneously generate the baryon asymmetry of the Universe and the Dark Matter abundance has been proposed. The Standard Model of particle physics succeeds to describe many physical processes and it has been tested to a great accuracy. However, it fails to provide a Dark Matter candidate, a so far undetected component of matter which makes up roughly 25% of the energy budget of the Universe. Furthermore, the question arises why there is a more matter (or baryons) than antimatter in the Universe taking into account that cosmology predicts a Universe with equal parts matter and anti-matter. The mechanism to generate a primordial matter-antimatter asymmetry is called baryogenesis. Any successful mechanism for baryogenesis needs to satisfy the three Sakharov conditions [2]: • violation of charge symmetry and of the combination of charge and parity symmetry • violation of baryon number • departure from thermal equilibrium In this paper [1] a new mechanism for the generation of a baryon asymmetry together with Dark Matter production has been proposed. The mechanism proposed to explain the observed baryon asymetry as well as the pro- duction of dark matter is developed around a fundamental ingredient: a new scalar particle Φ. The Φ particle is massive and would dominate the energy density of the Universe after inflation but prior to the Bing Bang nucleosynthesis. The same particle will directly decay, out of thermal equilibrium, to b=¯b quarks and if the Universe is cool enough ∼ O(10 MeV), the produced b quarks can hadronize and form B-mesons. -
Atomic Electric Dipole Moments and Cp Violation
261 ATOMIC ELECTRIC DIPOLE MOMENTS AND CP VIOLATION S.M.Barr Bartol Research Institute University of Delaware Newark, DE 19716 USA Abstract The subject of atomic electric dipole moments, the rapid recent progress in searching for them, and their significance for fundamental issues in particle theory is surveyed. particular it is shown how the edms of different kinds of atoms and molecules, as well Inas of the neutron, give vital information on the nature and origin of CP violation. Special stress is laid on supersymmetric theories and their consequences. 262 I. INTRODUCTION In this talk I am going to discuss atomic and molecular electric dipole moments (edms) from a particle theorist's point of view. The first and fundamental point is that permanent electric dipole moments violate both P and T. If we assume, as we are entitled to do, that OPT is conserved then we may speak equivalently of T-violation and OP-violation. I will mostly use the latter designation. That a permanent edm violates T is easily shown. Consider a proton. It has a magnetic dipole moment oriented along its spin axis. Suppose it also has an electric edm oriented, say, parallel to the magnetic dipole. Under T the electric dipole is not changed, as the spatial charge distribution is unaffected. But the magnetic dipole changes sign because current flows are reversed by T. Thus T takes a proton with parallel electric and magnetic dipoles into one with antiparallel moments. Now, if T is assumed to be an exact symmetry these two experimentally distinguishable kinds of proton will have the same mass. -
Introduction to Flavour Physics
Introduction to flavour physics Y. Grossman Cornell University, Ithaca, NY 14853, USA Abstract In this set of lectures we cover the very basics of flavour physics. The lec- tures are aimed to be an entry point to the subject of flavour physics. A lot of problems are provided in the hope of making the manuscript a self-study guide. 1 Welcome statement My plan for these lectures is to introduce you to the very basics of flavour physics. After the lectures I hope you will have enough knowledge and, more importantly, enough curiosity, and you will go on and learn more about the subject. These are lecture notes and are not meant to be a review. In the lectures, I try to talk about the basic ideas, hoping to give a clear picture of the physics. Thus many details are omitted, implicit assumptions are made, and no references are given. Yet details are important: after you go over the current lecture notes once or twice, I hope you will feel the need for more. Then it will be the time to turn to the many reviews [1–10] and books [11, 12] on the subject. I try to include many homework problems for the reader to solve, much more than what I gave in the actual lectures. If you would like to learn the material, I think that the problems provided are the way to start. They force you to fully understand the issues and apply your knowledge to new situations. The problems are given at the end of each section. -
Outline of Lecture 2 Baryon Asymmetry of the Universe. What's
Outline of Lecture 2 Baryon asymmetry of the Universe. What’s the problem? Electroweak baryogenesis. Electroweak baryon number violation Electroweak transition What can make electroweak mechanism work? Dark energy Baryon asymmetry of the Universe There is matter and no antimatter in the present Universe. Baryon-to-photon ratio, almost constant in time: nB 10 ηB = 6 10− ≡ nγ · Baryon-to-entropy, constant in time: n /s = 0.9 10 10 B · − What’s the problem? Early Universe (T > 1012 K = 100 MeV): creation and annihilation of quark-antiquark pairs ⇒ n ,n n q q¯ ≈ γ Hence nq nq¯ 9 − 10− nq + nq¯ ∼ How was this excess generated in the course of the cosmological evolution? Sakharov conditions To generate baryon asymmetry, three necessary conditions should be met at the same cosmological epoch: B-violation C-andCP-violation Thermal inequilibrium NB. Reservation: L-violation with B-conservation at T 100 GeV would do as well = Leptogenesis. & ⇒ Can baryon asymmetry be due to electroweak physics? Baryon number is violated in electroweak interactions. Non-perturbative effect Hint: triangle anomaly in baryonic current Bµ : 2 µ 1 gW µνλρ a a ∂ B = 3colors 3generations ε F F µ 3 · · · 32π2 µν λρ ! "Bq a Fµν: SU(2)W field strength; gW : SU(2)W coupling Likewise, each leptonic current (n = e, µ,τ) g2 ∂ Lµ = W ε µνλρFa Fa µ n 32π2 · µν λρ a 1 Large field fluctuations, Fµν ∝ gW− may have g2 Q d3xdt W ε µνλρFa Fa = 0 ≡ 32 2 · µν λρ ' # π Then B B = d3xdt ∂ Bµ =3Q fin− in µ # Likewise L L =Q n, fin− n, in B is violated, B L is not. -
TASI Lectures on the Strong CP Problem and Axions Pos(TASI2018)004 Is Θ
TASI Lectures on the Strong CP Problem and Axions PoS(TASI2018)004 Anson Hook∗ University of Maryland E-mail: hook at umd.edu These TASI lectures where given in 2018 and provide an introduction to the Strong CP problem and the axion. I start by introducing the Strong CP problem from both a classical and a quantum mechanical perspective, calculating the neutron eDM and discussing the q vacua. Next, I review the various solutions and discuss the active areas of axion model building. Finally, I summarize various experiments proposed to look for these solutions. Theoretical Advanced Study Institute Summer School 2018 ’Theory in an Era of Data’(TASI2018) 4 - 29 June, 2018 Boulder, Colorado ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). https://pos.sissa.it/ TASI Lectures on the Strong CP Problem and Axions Anson Hook 1. Introduction In these lectures, I will review the Strong CP problem, its solutions, active areas of research and the various experiments searching for the axion. The hope is that this set of lectures will provide a beginning graduate student with all of the requisite background need to start a Strong CP related project. As with any introduction to a topic, these notes will have much of my own personal bias on the subject so it is highly encouraged for readers to develop their own opinions. I will attempt to provide as many references as I can, but given my own laziness there will be references that I miss. -
A Scheme for Radiative CP Violation
A scheme for radiative CP violation Darwin Chang(1,2,3,4) and Wai-Yee Keung(2,3) (1)Physics Department, National Tsing-Hua University, Hsinchu, Taiwan (2)Department of Physics, University of Illinois at Chicago, Illinois 60607–7059 (3)High Energy Physics Division, Argonne National Laboratory, Illinois 60439–4815 (4)Institute of Physics, Academia Sinica, Taipei, Taiwan Abstract We present a simple model in which CP symmetry is spontaneously broken only after the radiative corrections are taken into account. The model includes two Higgs- arXiv:hep-ph/9409435v1 29 Sep 1994 boson doublets and two right-handed singlet neutrinos which induce the necessary non-hermitian interaction. To evade the Georgi-Pais theorem, some fine-tuning of coupling constants is necessary. However, we show that such fine-tuning is natural in the technical sense as it is protected by symmetry. Some phenomenological consequences are also discussed. PACS numbers: 11.30.Er, 14.80.Er More than thirty years after its experimental discovery, the origin of CP violation still remains very much a mystery. In the widely accepted Standard Model and many other models, CP violation is a result of the complex parameters[1] allowed in the La- grangian. For many physicists, such mundane explanation of the origin of the violation of CP symmetry is not very satisfactory. In an effort to understand it at a deeper level, many different schemes have been conceived in the literature. A popular alternative is to require CP symmetry at the Lagrangian level and allow its nonconservation only in the vacuum. Such scheme are commonly termed spontaneous CP violation[2]. -
Search for CP Violation in D 0 → Π Π Π Decays with the Energy Test Arxiv
EUROPEAN ORGANIZATION FOR NUCLEAR RESEARCH (CERN) CERN-PH-EP-2014-251 LHCb-PAPER-2014-054 14 October 2014 Search for CP violation in D0 ! π−π+π0 decays with the energy test The LHCb collaborationy Abstract A search for time-integrated CP violation in the Cabibbo-suppressed decay D0 ! π−π+π0 is performed using for the first time an unbinned model-independent technique known as the energy test. Using proton-proton collision data, corresponding to an integrated luminosity of 2:0 fb−1 collected by the p LHCb detector at a centre-of-mass energy of s = 8 TeV, the world's best sensitivity to CP violation in this decay is obtained. The data are found to be consistent with the hypothesis of CP symmetry with a p-value of (2:6 ± 0:5)%. arXiv:1410.4170v2 [hep-ex] 11 Dec 2014 Submitted to Phys. Lett. B c CERN on behalf of the LHCb collaboration, license CC-BY-4.0. yAuthors are listed at the end of this paper. ii 1 Introduction ging of the D mesons is performed through the measurement of the soft pion (πs) charge in the The decay D0 ! π−π+π0 (charge conjugate decays ∗+ 0 + D ! D πs decay. are implied unless stated otherwise) proceeds via a The method exploited in this Letter, called the singly Cabibbo-suppressed c! dud transition with energy test [6, 7], verifies the compatibility of the a possible admixture from a penguin amplitude. observed data with CP symmetry. It is sensitive The interference of these amplitudes may give rise to local CP violation in the Dalitz plot and not to to a violation of the charge-parity symmetry (CP global asymmetries. -
First Measurement of the Charge Asymmetry in Beauty-Quark Pair Production at a Hadron Collider
EUROPEAN ORGANIZATION FOR NUCLEAR RESEARCH (CERN) CERN-PH-EP-2014-130 LHCb-PAPER-2014-023 September 10, 2014 First measurement of the charge asymmetry in beauty-quark pair production at a hadron collider The LHCb collaborationy Abstract The difference in the angular distributions between beauty quarks and antiquarks, referred to as the charge asymmetry, is measured for the first time in bb pair production at a hadron collider. The data used correspond to an integrated luminosity of 1.0 fb−1 collected at 7 TeV center-of-mass energy in proton-proton collisions with the LHCb detector. The measurement is performed in three regions of the invariant mass of the bb system. The results obtained are b¯b 2 AC (40 < Mb¯b < 75 GeV=c ) = 0:4 ± 0:4 (stat) ± 0:3 (syst)%; b¯b 2 AC (75 < Mb¯b < 105 GeV=c ) = 2:0 ± 0:9 (stat) ± 0:6 (syst)%; b¯b 2 AC (Mb¯b > 105 GeV=c ) = 1:6 ± 1:7 (stat) ± 0:6 (syst)%; b¯b where AC is defined as the asymmetry in the difference in rapidity between jets formed from the beauty quark and antiquark. The beauty jets are required to satisfy 2 < η < 4, ET > 20 GeV, and have an opening angle in the transverse plane ∆φ > 2:6 rad. These measurements are arXiv:1406.4789v2 [hep-ex] 13 Sep 2014 consistent with the predictions of the Standard Model. c CERN on behalf of the LHCb collaboration, license CC-BY-3.0. yAuthors are listed on the following pages. ii LHCb collaboration R.