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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. -
Stephen Hawking and Leonard Mlodinow on the Grand Design
Book Reviews this if they are to make a significant con- before the creation’ (50). However, then tribution to the interface between science he says, ‘That is a possible model, which and faith. The rather good bibliography is favoured by those who maintain that at the end of this book would be a guide the account given in Genesis is literally to the competition – there are some excel- true’, but the big bang theory is ‘more lent books in this area already. Not rec- useful’, even though neither model is ommended. ‘more real than the other’ (50-51). This is deeply confusing not least because (a) Paul Wraight has retired from teach- Augustine himself did not take Genesis ing physics and electronics at literally, and (b) Augustine’s view is Aberdeen University and is thinking entirely compatible with the big bang and writing about design. theory! However, notwithstanding what comes later, Hawking admits at this Stephen Hawking and Leonard point that it is not clear that we can take Mlodinow time back beyond the big bang because The Grand Design: New Answers to the present laws of physics may break the Ultimate Questions of Life down (51). London: Bantam Press, 2010. 200 pp. hb. Hawking informs us that the 219 here- £18.99. ISBN-13 978-0593058299 sies condemned by Bishop Tempier of Paris in 1277 included the idea that This book was notoriously heralded by a nature follows laws, because this would front page splash in The Times headlined conflict with God’s omnipotence (24-25). ‘Hawking: God did not create Universe’. -
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). -
Arxiv:1202.4545V2 [Physics.Hist-Ph] 23 Aug 2012
The Relativity of Existence Stuart B. Heinrich [email protected] October 31, 2018 Abstract Despite the success of modern physics in formulating mathematical theories that can predict the outcome of experiments, we have made remarkably little progress towards answering the most fundamental question of: why is there a universe at all, as opposed to nothingness? In this paper, it is shown that this seemingly mind-boggling question has a simple logical answer if we accept that existence in the universe is nothing more than mathematical existence relative to the axioms of our universe. This premise is not baseless; it is shown here that there are indeed several independent strong logical arguments for why we should believe that mathematical existence is the only kind of existence. Moreover, it is shown that, under this premise, the answers to many other puzzling questions about our universe come almost immediately. Among these questions are: why is the universe apparently fine-tuned to be able to support life? Why are the laws of physics so elegant? Why do we have three dimensions of space and one of time, with approximate locality and causality at macroscopic scales? How can the universe be non-local and non-causal at the quantum scale? How can the laws of quantum mechanics rely on true randomness? 1 Introduction can seem astonishing that anything exists” [73, p.24]. Most physicists and cosmologists are equally perplexed. Over the course of modern history, we have seen advances in Richard Dawkins has called it a “searching question that biology, chemistry, physics and cosmology that have painted rightly calls for an explanatory answer” [26, p.155], and Sam an ever-clearer picture of how we came to exist in this uni- Harris says that “any intellectually honest person will admit verse. -
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. -
Communications-Mathematics and Applied Mathematics/Download/8110
A Mathematician's Journey to the Edge of the Universe "The only true wisdom is in knowing you know nothing." ― Socrates Manjunath.R #16/1, 8th Main Road, Shivanagar, Rajajinagar, Bangalore560010, Karnataka, India *Corresponding Author Email: [email protected] *Website: http://www.myw3schools.com/ A Mathematician's Journey to the Edge of the Universe What’s the Ultimate Question? Since the dawn of the history of science from Copernicus (who took the details of Ptolemy, and found a way to look at the same construction from a slightly different perspective and discover that the Earth is not the center of the universe) and Galileo to the present, we (a hoard of talking monkeys who's consciousness is from a collection of connected neurons − hammering away on typewriters and by pure chance eventually ranging the values for the (fundamental) numbers that would allow the development of any form of intelligent life) have gazed at the stars and attempted to chart the heavens and still discovering the fundamental laws of nature often get asked: What is Dark Matter? ... What is Dark Energy? ... What Came Before the Big Bang? ... What's Inside a Black Hole? ... Will the universe continue expanding? Will it just stop or even begin to contract? Are We Alone? Beginning at Stonehenge and ending with the current crisis in String Theory, the story of this eternal question to uncover the mysteries of the universe describes a narrative that includes some of the greatest discoveries of all time and leading personalities, including Aristotle, Johannes Kepler, and Isaac Newton, and the rise to the modern era of Einstein, Eddington, and Hawking. -
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. -
Conceptual Problems in Cosmology
Conceptual Problems in Cosmology F. J. Amaral Vieira Departamento de F´ısica, Universidade Estadual Vale do Acara´u(UVA) Avenida Dr. Guarani 317, CEP 62040-730, Sobral, Cear´a,Brazil e-mail: [email protected] (Dated: November 14, 2011) In this essay a critical review of present conceptual problems in current cosmology is provided from a more philosophical point of view. In essence, a digression on how could philosophy help cosmologists in what is strictly their fundamental endeavor is presented. We start by recalling some examples of enduring confrontations among philosophers and physicists on what could be contributed by the formers to the day-time striving of the second ones. Then, a short review of the standard model Friedmann-Lema^ıtre-Robertson-Walter (FLRW) of cosmology is given, since Einsteins days throughout the Hubble discover of the expansion of the universe, the Gamow, Alpher and Herman primordial nucleo-synthesis calculations and prediction of the cosmic microwave background (CMB) radiation; as detected by Penzias and Wilson, to Guth-Linde inflationary scenarios and the controversial multiverse and landscape ideas as prospective way outs to most cosmic conceptual conundrums. It seems apparent that cosmology is living a golden age with the advent of observations of high precision. Nonetheless, a critical revisiting of the direction in which it should go on appears also needed, for misconcepts like \quantum backgrounds for cosmological classical settings" and \quantum gravity unification” have not been properly constructed up-to-date. Thus, knowledge-building in cosmology, more than in any other field, should begin with visions of the reality, then taking technical form whenever concepts and relations inbetween are translated into a mathematical structure. -
Kaon Oscillations and Baryon Asymmetry of the Universe Abstract
Kaon oscillations and baryon asymmetry of the universe Wanpeng Tan∗ Department of Physics, Institute for Structure and Nuclear Astrophysics (ISNAP), and Joint Institute for Nuclear Astrophysics - Center for the Evolution of Elements (JINA-CEE), University of Notre Dame, Notre Dame, Indiana 46556, USA (Dated: September 17, 2019) Abstract Baryon asymmetry of the universe (BAU) can likely be explained with K0 − K00 oscillations of a newly developed mirror-matter model and new understanding of quantum chromodynamics (QCD) phase transitions. A consistent picture for the origin of both BAU and dark matter is presented with the aid of n − n0 oscillations of the new model. The global symmetry breaking transitions in QCD are proposed to be staged depending on condensation temperatures of strange, charm, bottom, and top quarks in the early universe. The long-standing BAU puzzle could then be understood with K0 − K00 oscillations that occur at the stage of strange quark condensation and baryon number violation via a non-perturbative sphaleron-like (coined \quarkiton") process. Similar processes at charm, bottom, and top quark condensation stages are also discussed including an interesting idea for top quark condensation to break both the QCD global Ut(1)A symmetry and the electroweak gauge symmetry at the same time. Meanwhile, the U(1)A or strong CP problem of particle physics is addressed with a possible explanation under the same framework. ∗ [email protected] 1 I. INTRODUCTION The matter-antimatter imbalance or baryon asymmetry of the universe (BAU) has been a long standing puzzle in the study of cosmology. Such an asymmetry can be quantified in various ways. -
Oilman at the Peak of Computers and Satellites to Numeri- Cal Predictions with Supercomputers
SPRING BOOKS COMMENT towards space observations and develop- ENERGY ing the use of computers in meteorology. From the findings of these three men, Fleming expertly weaves a tapestry of broader developments, from early uses Oilman at the peak of computers and satellites to numeri- cal predictions with supercomputers. He Gregor Macdonald applauds a biography of prescient explores intentional weather modification, geologist and energy theorist Marion King Hubbert. radioactive fallout, rocketry, air pollution and electromagnetism. For example, the air movements made apparent when scientist’s work does not always The Oracle of Oil: A researchers tracked the fallout from intersect neatly with the events of Maverick Geologist’s nuclear-bomb tests in the 1950s provided their time, but that was the good Quest for a Sustainable insight into atmospheric circulation. Afortune of US geologist and oilman Marion Future MASON INMAN The penultimate chapter covers what King Hubbert (1903–89). After labouring W. W. Norton: 2016. Fleming calls the birth of atmospheric for decades to perfect forecasting of the oil- science in the late 1950s, coinciding with production limit, he saw his efforts validated planning for the International Geophysical in the energy crises of the early 1970s. His Year in 1957–58. In 1956, Rossby proposed approach would later be known as Hubbert enlarging the definition of meteorology peak theory. shortage of ambition, Hubbert saw geology as to include elements such as atmospheric Journalist Mason Inman’s meticulous a wide-open field, and gate-crashed it. With chemistry and relevant biological pro- biography The Oracle of Oil follows Hub- precocious brilliance, he began to identify cesses. -
Large Lepton Asymmetry and the Cosmic QCD Transition
Large Lepton Asymmetry and the Cosmic QCD Transition Dissertation submitted to the Faculty of Physics, Bielefeld University by Mandy Maria Wygas December 2018 Supervisor and 1. assessor: Prof. Dr. Dietrich Bödeker 2. assessor: Prof. Dr. Dominik J. Schwarz Für Arne Abstract The lepton asymmetry of the universe is just weakly constraint and might be orders of magnitude larger than the baryon asymmetry. In this thesis, we investigate how a lepton asymmetry influences the cosmic trajectory through the phase diagram of Quantum Chromodynamics (QCD). Therefore, we de- velop a technique to determine the temperature evolution of chemical poten- tials during the QCD epoch of the early universe at arbitrary lepton flavor asymmetries. We will rely on an ideal quark gas approximation at high tem- peratures, T > 150 MeV, and a hadron resonance gas model at low temper- atures, T < 250 MeV. Higher-order perturbative corrections are (partially) included in the ideal quark gas approximation. To interpolate between these approximations, we will for the first time use lattice QCD susceptibilities to properly account for strong interaction effects close to the QCD transi- tion temperature TQCD. We therefore use a Taylor series ansatz of the QCD pressure up to second order in the chemical potentials. With this technique we investigate the impact of equally and unequally distributed lepton flavor asymmetries on the cosmic trajectory. We conclude with an estimate on the reliability of our technique via using a Taylor series of the QCD pressure. Gedruckt auf alterungsbeständigem Papier °° ISO 9706 Published work Parts of the methods and results discussed in Chapters 6 and 7 of this thesis have been published under [1]: M.