Emergent Particle Physics and the Cosmological Constant Puzzle
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The Five Common Particles
The Five Common Particles The world around you consists of only three particles: protons, neutrons, and electrons. Protons and neutrons form the nuclei of atoms, and electrons glue everything together and create chemicals and materials. Along with the photon and the neutrino, these particles are essentially the only ones that exist in our solar system, because all the other subatomic particles have half-lives of typically 10-9 second or less, and vanish almost the instant they are created by nuclear reactions in the Sun, etc. Particles interact via the four fundamental forces of nature. Some basic properties of these forces are summarized below. (Other aspects of the fundamental forces are also discussed in the Summary of Particle Physics document on this web site.) Force Range Common Particles It Affects Conserved Quantity gravity infinite neutron, proton, electron, neutrino, photon mass-energy electromagnetic infinite proton, electron, photon charge -14 strong nuclear force ≈ 10 m neutron, proton baryon number -15 weak nuclear force ≈ 10 m neutron, proton, electron, neutrino lepton number Every particle in nature has specific values of all four of the conserved quantities associated with each force. The values for the five common particles are: Particle Rest Mass1 Charge2 Baryon # Lepton # proton 938.3 MeV/c2 +1 e +1 0 neutron 939.6 MeV/c2 0 +1 0 electron 0.511 MeV/c2 -1 e 0 +1 neutrino ≈ 1 eV/c2 0 0 +1 photon 0 eV/c2 0 0 0 1) MeV = mega-electron-volt = 106 eV. It is customary in particle physics to measure the mass of a particle in terms of how much energy it would represent if it were converted via E = mc2. -
Fundamentals of Particle Physics
Fundamentals of Par0cle Physics Particle Physics Masterclass Emmanuel Olaiya 1 The Universe u The universe is 15 billion years old u Around 150 billion galaxies (150,000,000,000) u Each galaxy has around 300 billion stars (300,000,000,000) u 150 billion x 300 billion stars (that is a lot of stars!) u That is a huge amount of material u That is an unimaginable amount of particles u How do we even begin to understand all of matter? 2 How many elementary particles does it take to describe the matter around us? 3 We can describe the material around us using just 3 particles . 3 Matter Particles +2/3 U Point like elementary particles that protons and neutrons are made from. Quarks Hence we can construct all nuclei using these two particles -1/3 d -1 Electrons orbit the nuclei and are help to e form molecules. These are also point like elementary particles Leptons We can build the world around us with these 3 particles. But how do they interact. To understand their interactions we have to introduce forces! Force carriers g1 g2 g3 g4 g5 g6 g7 g8 The gluon, of which there are 8 is the force carrier for nuclear forces Consider 2 forces: nuclear forces, and electromagnetism The photon, ie light is the force carrier when experiencing forces such and electricity and magnetism γ SOME FAMILAR THE ATOM PARTICLES ≈10-10m electron (-) 0.511 MeV A Fundamental (“pointlike”) Particle THE NUCLEUS proton (+) 938.3 MeV neutron (0) 939.6 MeV E=mc2. Einstein’s equation tells us mass and energy are equivalent Wave/Particle Duality (Quantum Mechanics) Einstein E -
Introduction to Particle Physics
SFB 676 – Projekt B2 Introduction to Particle Physics Christian Sander (Universität Hamburg) DESY Summer Student Lectures – Hamburg – 20th July '11 Outline ● Introduction ● History: From Democrit to Thomson ● The Standard Model ● Gauge Invariance ● The Higgs Mechanism ● Symmetries … Break ● Shortcomings of the Standard Model ● Physics Beyond the Standard Model ● Recent Results from the LHC ● Outlook Disclaimer: Very personal selection of topics and for sure many important things are left out! 20th July '11 Introduction to Particle Physics 2 20th July '11 Introduction to Particle PhysicsX Files: Season 2, Episode 233 … für Chester war das nur ein Weg das Geld für das eigentlich theoretische Zeugs aufzubringen, was ihn interessierte … die Erforschung Dunkler Materie, …ähm… Quantenpartikel, Neutrinos, Gluonen, Mesonen und Quarks. Subatomare Teilchen Die Geheimnisse des Universums! Theoretisch gesehen sind sie sogar die Bausteine der Wirklichkeit ! Aber niemand weiß, ob sie wirklich existieren !? 20th July '11 Introduction to Particle PhysicsX Files: Season 2, Episode 234 The First Particle Physicist? By convention ['nomos'] sweet is sweet, bitter is bitter, hot is hot, cold is cold, color is color; but in truth there are only atoms and the void. Democrit, * ~460 BC, †~360 BC in Abdera Hypothesis: ● Atoms have same constituents ● Atoms different in shape (assumption: geometrical shapes) ● Iron atoms are solid and strong with hooks that lock them into a solid ● Water atoms are smooth and slippery ● Salt atoms, because of their taste, are sharp and pointed ● Air atoms are light and whirling, pervading all other materials 20th July '11 Introduction to Particle Physics 5 Corpuscular Theory of Light Light consist out of particles (Newton et al.) ↕ Light is a wave (Huygens et al.) ● Mainly because of Newtons prestige, the corpuscle theory was widely accepted (more than 100 years) Sir Isaac Newton ● Failing to describe interference, diffraction, and *1643, †1727 polarization (e.g. -
Naturalness and New Approaches to the Hierarchy Problem
Naturalness and New Approaches to the Hierarchy Problem PiTP 2017 Nathaniel Craig Department of Physics, University of California, Santa Barbara, CA 93106 No warranty expressed or implied. This will eventually grow into a more polished public document, so please don't disseminate beyond the PiTP community, but please do enjoy. Suggestions, clarifications, and comments are welcome. Contents 1 Introduction 2 1.0.1 The proton mass . .3 1.0.2 Flavor hierarchies . .4 2 The Electroweak Hierarchy Problem 5 2.1 A toy model . .8 2.2 The naturalness strategy . 13 3 Old Hierarchy Solutions 16 3.1 Lowered cutoff . 16 3.2 Symmetries . 17 3.2.1 Supersymmetry . 17 3.2.2 Global symmetry . 22 3.3 Vacuum selection . 26 4 New Hierarchy Solutions 28 4.1 Twin Higgs / Neutral naturalness . 28 4.2 Relaxion . 31 4.2.1 QCD/QCD0 Relaxion . 31 4.2.2 Interactive Relaxion . 37 4.3 NNaturalness . 39 5 Rampant Speculation 42 5.1 UV/IR mixing . 42 6 Conclusion 45 1 1 Introduction What are the natural sizes of parameters in a quantum field theory? The original notion is the result of an aggregation of different ideas, starting with Dirac's Large Numbers Hypothesis (\Any two of the very large dimensionless numbers occurring in Nature are connected by a simple mathematical relation, in which the coefficients are of the order of magnitude unity" [1]), which was not quantum in nature, to Gell- Mann's Totalitarian Principle (\Anything that is not compulsory is forbidden." [2]), to refinements by Wilson and 't Hooft in more modern language. -
Quantum Field Theory*
Quantum Field Theory y Frank Wilczek Institute for Advanced Study, School of Natural Science, Olden Lane, Princeton, NJ 08540 I discuss the general principles underlying quantum eld theory, and attempt to identify its most profound consequences. The deep est of these consequences result from the in nite number of degrees of freedom invoked to implement lo cality.Imention a few of its most striking successes, b oth achieved and prosp ective. Possible limitation s of quantum eld theory are viewed in the light of its history. I. SURVEY Quantum eld theory is the framework in which the regnant theories of the electroweak and strong interactions, which together form the Standard Mo del, are formulated. Quantum electro dynamics (QED), b esides providing a com- plete foundation for atomic physics and chemistry, has supp orted calculations of physical quantities with unparalleled precision. The exp erimentally measured value of the magnetic dip ole moment of the muon, 11 (g 2) = 233 184 600 (1680) 10 ; (1) exp: for example, should b e compared with the theoretical prediction 11 (g 2) = 233 183 478 (308) 10 : (2) theor: In quantum chromo dynamics (QCD) we cannot, for the forseeable future, aspire to to comparable accuracy.Yet QCD provides di erent, and at least equally impressive, evidence for the validity of the basic principles of quantum eld theory. Indeed, b ecause in QCD the interactions are stronger, QCD manifests a wider variety of phenomena characteristic of quantum eld theory. These include esp ecially running of the e ective coupling with distance or energy scale and the phenomenon of con nement. -
Solving the Hierarchy Problem
solving the hierarchy problem Joseph Lykken Fermilab/U. Chicago puzzle of the day: why is gravity so weak? answer: because there are large or warped extra dimensions about to be discovered at colliders puzzle of the day: why is gravity so weak? real answer: don’t know many possibilities may not even be a well-posed question outline of this lecture • what is the hierarchy problem of the Standard Model • is it really a problem? • what are the ways to solve it? • how is this related to gravity? what is the hierarchy problem of the Standard Model? • discuss concepts of naturalness and UV sensitivity in field theory • discuss Higgs naturalness problem in SM • discuss extra assumptions that lead to the hierarchy problem of SM UV sensitivity • Ken Wilson taught us how to think about field theory: “UV completion” = high energy effective field theory matching scale, Λ low energy effective field theory, e.g. SM energy UV sensitivity • how much do physical parameters of the low energy theory depend on details of the UV matching (i.e. short distance physics)? • if you know both the low and high energy theories, can answer this question precisely • if you don’t know the high energy theory, use a crude estimate: how much do the low energy observables change if, e.g. you let Λ → 2 Λ ? degrees of UV sensitivity parameter UV sensitivity “finite” quantities none -- UV insensitive dimensionless couplings logarithmic -- UV insensitive e.g. gauge or Yukawa couplings dimension-full coefs of higher dimension inverse power of cutoff -- “irrelevant” operators e.g. -
A Young Physicist's Guide to the Higgs Boson
A Young Physicist’s Guide to the Higgs Boson Tel Aviv University Future Scientists – CERN Tour Presented by Stephen Sekula Associate Professor of Experimental Particle Physics SMU, Dallas, TX Programme ● You have a problem in your theory: (why do you need the Higgs Particle?) ● How to Make a Higgs Particle (One-at-a-Time) ● How to See a Higgs Particle (Without fooling yourself too much) ● A View from the Shadows: What are the New Questions? (An Epilogue) Stephen J. Sekula - SMU 2/44 You Have a Problem in Your Theory Credit for the ideas/example in this section goes to Prof. Daniel Stolarski (Carleton University) The Usual Explanation Usual Statement: “You need the Higgs Particle to explain mass.” 2 F=ma F=G m1 m2 /r Most of the mass of matter lies in the nucleus of the atom, and most of the mass of the nucleus arises from “binding energy” - the strength of the force that holds particles together to form nuclei imparts mass-energy to the nucleus (ala E = mc2). Corrected Statement: “You need the Higgs Particle to explain fundamental mass.” (e.g. the electron’s mass) E2=m2 c4+ p2 c2→( p=0)→ E=mc2 Stephen J. Sekula - SMU 4/44 Yes, the Higgs is important for mass, but let’s try this... ● No doubt, the Higgs particle plays a role in fundamental mass (I will come back to this point) ● But, as students who’ve been exposed to introductory physics (mechanics, electricity and magnetism) and some modern physics topics (quantum mechanics and special relativity) you are more familiar with.. -
On Particle Physics
On Particle Physics Searching for the Fundamental US ATLAS The continuing search for the basic building blocks of matter is the US ATLAS subject of Particle Physics (also called High Energy Physics). The idea of fundamental building blocks has evolved from the concept of four elements (earth, air, fire and water) of the Ancient Greeks to the nineteenth century picture of atoms as tiny “billiard balls.” The key word here is FUNDAMENTAL — objects which are simple and have no structure — they are not made of anything smaller! Our current understanding of these fundamental constituents began to fall into place around 100 years ago, when experimenters first discovered that the atom was not fundamental at all, but was itself made of smaller building blocks. Using particle probes as “microscopes,” scientists deter- mined that an atom has a dense center, or NUCLEUS, of positive charge surrounded by a dilute “cloud” of light, negatively- charged electrons. In between the nucleus and electrons, most of the atom is empty space! As the particle “microscopes” became more and more powerful, scientists found that the nucleus was composed of two types of yet smaller constituents called protons and neutrons, and that even pro- tons and neutrons are made up of smaller particles called quarks. The quarks inside the nucleus come in two varieties, called “up” or u-quark and “down” or d-quark. As far as we know, quarks and electrons really are fundamental (although experimenters continue to look for evidence to the con- trary). We know that these fundamental building blocks are small, but just how small are they? Using probes that can “see” down to very small distances inside the atom, physicists know that quarks and electrons are smaller than 10-18 (that’s 0.000 000 000 000 000 001! ) meters across. -
A Modified Naturalness Principle and Its Experimental Tests
A modified naturalness principle and its experimental tests Marco Farinaa, Duccio Pappadopulob;c and Alessandro Strumiad;e (a) Department of Physics, LEPP, Cornell University, Ithaca, NY 14853, USA (b) Department of Physics, University of California, Berkeley, CA 94720, USA (c) Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, USA (d) Dipartimento di Fisica dell’Universita` di Pisa and INFN, Italia (e) National Institute of Chemical Physics and Biophysics, Tallinn, Estonia Abstract Motivated by LHC results, we modify the usual criterion for naturalness by ig- noring the uncomputable power divergences. The Standard Model satisfies the modified criterion (‘finite naturalness’) for the measured values of its parameters. Extensions of the SM motivated by observations (Dark Matter, neutrino masses, the strong CP problem, vacuum instability, inflation) satisfy finite naturalness in special ranges of their parameter spaces which often imply new particles below a few TeV. Finite naturalness bounds are weaker than usual naturalness bounds because any new particle with SM gauge interactions gives a finite contribution to the Higgs mass at two loop order. Contents 1 Introduction2 2 The Standard Model3 3 Finite naturalness, neutrino masses and leptogenesis4 3.1 Type-I see saw . .5 3.2 Type-III see saw . .6 3.3 Type-II see saw . .6 arXiv:1303.7244v3 [hep-ph] 29 Apr 2014 4 Finite naturalness and Dark Matter7 4.1 Minimal Dark Matter . .7 4.2 The scalar singlet DM model . 10 4.3 The fermion singlet model . 10 5 Finite naturalness and axions 13 5.1 KSVZ axions . 13 5.2 DFSZ axions . 14 6 Finite naturalness, vacuum decay and inflation 14 7 Conclusions 15 1 1 Introduction The naturalness principle strongly influenced high-energy physics in the past decades [1], leading to the belief that physics beyond the Standard Model (SM) must exist at a scale ΛNP such that quadratically divergent quantum corrections to the Higgs squared mass are made finite (presumably up to a log divergence) and not much larger than the Higgs mass Mh itself. -
Particle Physics Dr Victoria Martin, Spring Semester 2012 Lecture 11: Mesons and Baryons
Particle Physics Dr Victoria Martin, Spring Semester 2012 Lecture 11: Mesons and Baryons !Measuring Jets !Fragmentation !Mesons and Baryons !Isospin and hypercharge !SU(3) flavour symmetry !Heavy Quark states 1 From Tuesday: Summary • In QCD, the coupling strength "S decreases at high momentum transfer (q2) increases at low momentum transfer. • Perturbation theory is only useful at high momentum transfer. • Non-perturbative techniques required at low momentum transfer. • At colliders, hard scatter produces quark, anti-quarks and gluons. • Fragmentation (hadronisation) describes how partons produced in hard scatter become final state hadrons. Need non-perturbative techniques. • Final state hadrons observed in experiments as jets. Measure jet pT, !, ! • Key measurement at lepton collider, evidence for NC=3 colours of quarks. + 2 σ(e e− hadrons) e R = → = N q σ(e+e µ+µ ) c e2 − → − • Next lecture: mesons and baryons! Griffiths chapter 5. 2 6 41. Plots of cross sections and related quantities + σ and R in e e− Collisions -2 10 ω φ J/ψ -3 10 ψ(2S) ρ Υ -4 ρ ! 10 Z -5 10 [mb] σ -6 R 10 -7 10 -8 10 2 1 10 10 Υ 3 10 J/ψ ψ(2S) Z 10 2 φ ω to theR Fermilab accelerator complex. In addition, both the CDF [11] and DØ detectors [12] 10 were upgraded. The resultsρ reported! here utilize an order of magnitude higher integrated luminosity1 than reported previously [5]. ρ -1 10 2 II. PERTURBATIVE1 QCD 10 10 √s [GeV] + + + + Figure 41.6: World data on the total cross section of e e− hadrons and the ratio R(s)=σ(e e− hadrons, s)/σ(e e− µ µ−,s). -
MIT at the Large Hadron Collider—Illuminating the High-Energy Frontier
Mit at the large hadron collider—Illuminating the high-energy frontier 40 ) roland | klute mit physics annual 2010 gunther roland and Markus Klute ver the last few decades, teams of physicists and engineers O all over the globe have worked on the components for one of the most complex machines ever built: the Large Hadron Collider (LHC) at the CERN laboratory in Geneva, Switzerland. Collaborations of thousands of scientists have assembled the giant particle detectors used to examine collisions of protons and nuclei at energies never before achieved in a labo- ratory. After initial tests proved successful in late 2009, the LHC physics program was launched in March 2010. Now the race is on to fulfill the LHC’s paradoxical mission: to complete the Stan- dard Model of particle physics by detecting its last missing piece, the Higgs boson, and to discover the building blocks of a more complete theory of nature to finally replace the Standard Model. The MIT team working on the Compact Muon Solenoid (CMS) experiment at the LHC stands at the forefront of this new era of particle and nuclear physics. The High Energy Frontier Our current understanding of the fundamental interactions of nature is encap- sulated in the Standard Model of particle physics. In this theory, the multitude of subatomic particles is explained in terms of just two kinds of basic building blocks: quarks, which form protons and neutrons, and leptons, including the electron and its heavier cousins. From the three basic interactions described by the Standard Model—the strong, electroweak and gravitational forces—arise much of our understanding of the world around us, from the formation of matter in the early universe, to the energy production in the Sun, and the stability of atoms and mit physics annual 2010 roland | klute ( 41 figure 1 A photograph of the interior, central molecules. -
Hep-Ph] 19 Nov 2018
The discreet charm of higgsino dark matter { a pocket review Kamila Kowalska∗ and Enrico Maria Sessoloy National Centre for Nuclear Research, Ho_za69, 00-681 Warsaw, Poland Abstract We give a brief review of the current constraints and prospects for detection of higgsino dark matter in low-scale supersymmetry. In the first part we argue, after per- forming a survey of all potential dark matter particles in the MSSM, that the (nearly) pure higgsino is the only candidate emerging virtually unscathed from the wealth of observational data of recent years. In doing so by virtue of its gauge quantum numbers and electroweak symmetry breaking only, it maintains at the same time a relatively high degree of model-independence. In the second part we properly review the prospects for detection of a higgsino-like neutralino in direct underground dark matter searches, col- lider searches, and indirect astrophysical signals. We provide estimates for the typical scale of the superpartners and fine tuning in the context of traditional scenarios where the breaking of supersymmetry is mediated at about the scale of Grand Unification and where strong expectations for a timely detection of higgsinos in underground detectors are closely related to the measured 125 GeV mass of the Higgs boson at the LHC. arXiv:1802.04097v3 [hep-ph] 19 Nov 2018 ∗[email protected] [email protected] 1 Contents 1 Introduction2 2 Dark matter in the MSSM4 2.1 SU(2) singlets . .5 2.2 SU(2) doublets . .7 2.3 SU(2) adjoint triplet . .9 2.4 Mixed cases . .9 3 Phenomenology of higgsino dark matter 12 3.1 Prospects for detection in direct and indirect searches .