Cosmological Evolution of Light Dark Photon Dark Matter
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Dark Energy and Dark Matter As Inertial Effects Introduction
Dark Energy and Dark Matter as Inertial Effects Serkan Zorba Department of Physics and Astronomy, Whittier College 13406 Philadelphia Street, Whittier, CA 90608 [email protected] ABSTRACT A disk-shaped universe (encompassing the observable universe) rotating globally with an angular speed equal to the Hubble constant is postulated. It is shown that dark energy and dark matter are cosmic inertial effects resulting from such a cosmic rotation, corresponding to centrifugal (dark energy), and a combination of centrifugal and the Coriolis forces (dark matter), respectively. The physics and the cosmological and galactic parameters obtained from the model closely match those attributed to dark energy and dark matter in the standard Λ-CDM model. 20 Oct 2012 Oct 20 ph] - PACS: 95.36.+x, 95.35.+d, 98.80.-k, 04.20.Cv [physics.gen Introduction The two most outstanding unsolved problems of modern cosmology today are the problems of dark energy and dark matter. Together these two problems imply that about a whopping 96% of the energy content of the universe is simply unaccounted for within the reigning paradigm of modern cosmology. arXiv:1210.3021 The dark energy problem has been around only for about two decades, while the dark matter problem has gone unsolved for about 90 years. Various ideas have been put forward, including some fantastic ones such as the presence of ghostly fields and particles. Some ideas even suggest the breakdown of the standard Newton-Einstein gravity for the relevant scales. Although some progress has been made, particularly in the area of dark matter with the nonstandard gravity theories, the problems still stand unresolved. -
Arxiv:1712.01768V1 [Hep-Ex] 5 Dec 2017
Prospects of the SHiP and NA62 experiments at CERN for hidden sector searches Philippe Mermod∗, on behalf of the SHiP Collaboration Particle Physics Department, Faculty of Science, University of Geneva, Geneva, Switzerland E-mail: [email protected] High-intensity proton beams impinging on a fixed target or beam dump allow to probe new physics via the production of new weakly-coupled particles in hadron decays. The CERN SPS provides opportunities to do so with the running NA62 experiment and the planned SHiP ex- periment. Reconstruction of kaon decay kinematics (beam mode) allows NA62 to probe for the existence of right-handed neutrinos and dark photons with masses below 0.45 GeV. Direct recon- struction of displaced vertices from the decays of new neutral particles (dump mode) will allow NA62 and SHiP to probe right-handed neutrinos with masses up to 5 GeV and mixings down to several orders of magnitude smaller than current constraints, in regions favoured in models which explain at once neutrino masses, matter-antimatter asymmetry and dark matter. arXiv:1712.01768v1 [hep-ex] 5 Dec 2017 The 19th International Workshop on Neutrinos from Accelerators-NUFACT2017 25-30 September, 2017 Uppsala University, Uppsala, Sweden ∗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/ Hidden sector searches with SHiP and NA62 Philippe Mermod 1. Introduction The LHC experiments have been running for several years without finding new physics at the TeV scale. A complementary approach is to probe the presence of new particles at lower energy scales with couplings to the Standard Model so weak that they have escaped detection in previous searches. -
Dark Matter and the Early Universe: a Review Arxiv:2104.11488V1 [Hep-Ph
Dark matter and the early Universe: a review A. Arbey and F. Mahmoudi Univ Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, Institut de Physique des 2 Infinis de Lyon, UMR 5822, 69622 Villeurbanne, France Theoretical Physics Department, CERN, CH-1211 Geneva 23, Switzerland Institut Universitaire de France, 103 boulevard Saint-Michel, 75005 Paris, France Abstract Dark matter represents currently an outstanding problem in both cosmology and particle physics. In this review we discuss the possible explanations for dark matter and the experimental observables which can eventually lead to the discovery of dark matter and its nature, and demonstrate the close interplay between the cosmological properties of the early Universe and the observables used to constrain dark matter models in the context of new physics beyond the Standard Model. arXiv:2104.11488v1 [hep-ph] 23 Apr 2021 1 Contents 1 Introduction 3 2 Standard Cosmological Model 3 2.1 Friedmann-Lema^ıtre-Robertson-Walker model . 4 2.2 A quick story of the Universe . 5 2.3 Big-Bang nucleosynthesis . 8 3 Dark matter(s) 9 3.1 Observational evidences . 9 3.1.1 Galaxies . 9 3.1.2 Galaxy clusters . 10 3.1.3 Large and cosmological scales . 12 3.2 Generic types of dark matter . 14 4 Beyond the standard cosmological model 16 4.1 Dark energy . 17 4.2 Inflation and reheating . 19 4.3 Other models . 20 4.4 Phase transitions . 21 5 Dark matter in particle physics 21 5.1 Dark matter and new physics . 22 5.1.1 Thermal relics . 22 5.1.2 Non-thermal relics . -
1 Standard Model: Successes and Problems
Searching for new particles at the Large Hadron Collider James Hirschauer (Fermi National Accelerator Laboratory) Sambamurti Memorial Lecture : August 7, 2017 Our current theory of the most fundamental laws of physics, known as the standard model (SM), works very well to explain many aspects of nature. Most recently, the Higgs boson, predicted to exist in the late 1960s, was discovered by the CMS and ATLAS collaborations at the Large Hadron Collider at CERN in 2012 [1] marking the first observation of the full spectrum of predicted SM particles. Despite the great success of this theory, there are several aspects of nature for which the SM description is completely lacking or unsatisfactory, including the identity of the astronomically observed dark matter and the mass of newly discovered Higgs boson. These and other apparent limitations of the SM motivate the search for new phenomena beyond the SM either directly at the LHC or indirectly with lower energy, high precision experiments. In these proceedings, the successes and some of the shortcomings of the SM are described, followed by a description of the methods and status of the search for new phenomena at the LHC, with some focus on supersymmetry (SUSY) [2], a specific theory of physics beyond the standard model (BSM). 1 Standard model: successes and problems The standard model of particle physics describes the interactions of fundamental matter particles (quarks and leptons) via the fundamental forces (mediated by the force carrying particles: the photon, gluon, and weak bosons). The Higgs boson, also a fundamental SM particle, plays a central role in the mechanism that determines the masses of the photon and weak bosons, as well as the rest of the standard model particles. -
7. Gamma and X-Ray Interactions in Matter
Photon interactions in matter Gamma- and X-Ray • Compton effect • Photoelectric effect Interactions in Matter • Pair production • Rayleigh (coherent) scattering Chapter 7 • Photonuclear interactions F.A. Attix, Introduction to Radiological Kinematics Physics and Radiation Dosimetry Interaction cross sections Energy-transfer cross sections Mass attenuation coefficients 1 2 Compton interaction A.H. Compton • Inelastic photon scattering by an electron • Arthur Holly Compton (September 10, 1892 – March 15, 1962) • Main assumption: the electron struck by the • Received Nobel prize in physics 1927 for incoming photon is unbound and stationary his discovery of the Compton effect – The largest contribution from binding is under • Was a key figure in the Manhattan Project, condition of high Z, low energy and creation of first nuclear reactor, which went critical in December 1942 – Under these conditions photoelectric effect is dominant Born and buried in • Consider two aspects: kinematics and cross Wooster, OH http://en.wikipedia.org/wiki/Arthur_Compton sections http://www.findagrave.com/cgi-bin/fg.cgi?page=gr&GRid=22551 3 4 Compton interaction: Kinematics Compton interaction: Kinematics • An earlier theory of -ray scattering by Thomson, based on observations only at low energies, predicted that the scattered photon should always have the same energy as the incident one, regardless of h or • The failure of the Thomson theory to describe high-energy photon scattering necessitated the • Inelastic collision • After the collision the electron departs -
Effective Description of Dark Matter As a Viscous Fluid
Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Effective Description of Dark Matter as a Viscous Fluid Nikolaos Tetradis University of Athens Work with: D. Blas, S. Floerchinger, M. Garny, U. Wiedemann . N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Distribution of dark and baryonic matter in the Universe Figure: 2MASS Galaxy Catalog (more than 1.5 million galaxies). N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Inhomogeneities Inhomogeneities are treated as perturbations on top of an expanding homogeneous background. Under gravitational attraction, the matter overdensities grow and produce the observed large-scale structure. The distribution of matter at various redshifts reflects the detailed structure of the cosmological model. Define the density field δ = δρ/ρ0 and its spectrum hδ(k)δ(q)i ≡ δD(k + q)P(k): . N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid 31 timation method in its entirety, but it should be equally valid. 7.3. Comparison to other results Figure 35 compares our results from Table 3 (modeling approach) with other measurements from galaxy surveys, but must be interpreted with care. The UZC points may contain excess large-scale power due to selection function effects (Padmanabhan et al. 2000; THX02), and the an- gular SDSS points measured from the early data release sample are difficult to interpret because of their extremely broad window functions. -
Glossary of Scientific Terms in the Mystery of Matter
GLOSSARY OF SCIENTIFIC TERMS IN THE MYSTERY OF MATTER Term Definition Section acid A substance that has a pH of less than 7 and that can react with 1 metals and other substances. air The mixture of oxygen, nitrogen, and other gasses that is consistently 1 present around us. alchemist A person who practices a form of chemistry from the Middle Ages 1 that was concerned with transforming various metals into gold. Alchemy A type of science and philosophy from the Middle Ages that 1 attempted to perform unusual experiments, taking something ordinary and turning it into something extraordinary. alkali metals Any of a group of soft metallic elements that form alkali solutions 3 when they combine with water. They include lithium, sodium, potassium, rubidium, cesium, and francium. alkaline earth Any of a group of metallic elements that includes beryllium, 3 metals magnesium, calcium, strontium, barium, and radium. alpha particle A positively charged particle, indistinguishable from a helium atom 5, 6 nucleus and consisting of two protons and two neutrons. alpha decay A type of radioactive decay in which a nucleus emits 6 an alpha particle. aplastic anemia A disorder of the bone marrow that results in too few blood cells. 4 apothecary The person in a pharmacy who distributes medicine. 1 atom The smallest component of an element that shares the chemical 1, 2, 3, 4, 5, 6 properties of the element and contains a nucleus with neutrons, protons, and electrons. atomic bomb A bomb whose explosive force comes from a chain reaction based on 6 nuclear fission. atomic number The number of protons in the nucleus of an atom. -
Review of Dark Matter
Review of Dark Matter Leonard S. Kisslinger Department of Physics, Carnegie Mellon University, Pittsburgh PA 15213 USA. Debasish Das Saha Institute of Nuclear Physics,1/AF, Bidhan Nagar, Kolkata 700064, INDIA. PACS Indices:11.30.Er,14.60.Lm,13.15.+g Keywords: dark matter, sterile neutrinos, dark photons Abstract In this review of Dark Matter we review dark matter as sterile neutrinos, fermions, with their present and possibly future detection via neutrino Oscillations. We review the creation of Dark Matter via interactions with the Dark Energy (quintesence) field. We also review bosons as dark matter, discussing a proposed search for dark photons. Since photons are vector bosons, if dark photons exist at least part of dark matter are vector bosons. Ongoing experimental detection of Dark Matter is reviewed. 1 Introduction The most important experiments which have estimated the amount of Dark Matter in the present universe are Cosmic Microwave Background Radiation (CMBR) experiments, discussed in the section 2. There have been a number of theoretical models for the creation of Dark Matter, which is reviewed in section 3. It is almost certain that sterile nuetrinos are part of Dark Matter. Experiments detecting sterile nuetrinos via neutrino oscillation and a theoretical study of neutrino oscil- lations with 3 active and 3 sterile neutrinos with the present results are discussed in section 4. Also a recent search for sub-Gev Dark Matter by the MiniBooNE-DM Collaboration is briefly discussed in section 4. Neutrinos are fermions with quantum spin 1/2. It is possible that some Dark Matter particle are vector bosons with quantum spin 1, like the photon. -
Light Dark Matter Searches with Positrons
Eur. Phys. J. A manuscript No. (will be inserted by the editor) Light dark matter searches with positrons M. Battaglieri1,2, A. Bianconi3,4, P. Bisio5, M. Bondì1, A. Celentano1, G. Costantini3,4, P.L. Cole6, L. Darmé7, R. De Vita1, A. D’Angelo8,9, M. De Napoli10, L. El Fassi11, V. Kozhuharov7,12, A. Italiano10, G. Krnjaic13,14, L. Lanza8, M. Leali3,4, L. Marsicano1,a, V. Mascagna4,15, S. Migliorati3,4, E. Nardi7, M. Raggi16,17,a, N. Randazzo10, E. Santopinto1, E. Smith2, M. Spreafico5, S. Stepanyan2, M. Ungaro2, P. Valente17, L. Venturelli3,4, M.H. Wood18 1Istituto Nazionale di Fisica Nucleare, Sezione di Genova, 16146 Genova, Italy 2Thomas Jefferson National Accelerator Facility, Newport News, Virginia 23606 3Università degli Studi di Brescia, 25123 Brescia, Italy 4INFN, Sezione di Pavia, 27100 Pavia, Italy 5Università degli Studi di Genova, 16146 Genova, Italy 6Lamar University, 4400 MLK Blvd, PO Box 10046, Beaumont, Texas 77710 7Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali di Frascati, Via E. Fermi 54, Frascati, Italy 8INFN, Sezione di Roma Tor Vergata, 00133 Rome, Italy 9Università di Roma Tor Vergata, 00133 Rome Italy 10Istituto Nazionale di Fisica Nucleare, Sezione di Catania, 95125 Catania, Italy 11Mississippi State University, Mississippi State, Mississippi 39762-5167, USA 12Faculty of physics, University of Sofia, 5 J. Bourchier Blvd., 1164 Sofia, Bulgaria 13Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA 14Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA 15Università degli Studi dell’Insubria, 22100 Como, Italy 16Sapienza Università di Roma, piazzale Aldo Moro 5 Roma, Italy 17Istituto Nazionale di Fisica Nucleare, Sezione di Roma, piazzale Aldo Moro 5 Roma, Italy 18Canisius College, Buffalo, NY 14208, USA Draft : May 27, 2021 Abstract We discuss two complementary strategies to 1 Introduction and motivations search for light dark matter (LDM) exploiting the posi- tron beam possibly available in the future at Jefferson One of the most compelling arguments motivating the Laboratory. -
Modified Newtonian Dynamics
J. Astrophys. Astr. (December 2017) 38:59 © Indian Academy of Sciences https://doi.org/10.1007/s12036-017-9479-0 Modified Newtonian Dynamics (MOND) as a Modification of Newtonian Inertia MOHAMMED ALZAIN Department of Physics, Omdurman Islamic University, Omdurman, Sudan. E-mail: [email protected] MS received 2 February 2017; accepted 14 July 2017; published online 31 October 2017 Abstract. We present a modified inertia formulation of Modified Newtonian dynamics (MOND) without retaining Galilean invariance. Assuming that the existence of a universal upper bound, predicted by MOND, to the acceleration produced by a dark halo is equivalent to a violation of the hypothesis of locality (which states that an accelerated observer is pointwise inertial), we demonstrate that Milgrom’s law is invariant under a new space–time coordinate transformation. In light of the new coordinate symmetry, we address the deficiency of MOND in resolving the mass discrepancy problem in clusters of galaxies. Keywords. Dark matter—modified dynamics—Lorentz invariance 1. Introduction the upper bound is inferred by writing the excess (halo) acceleration as a function of the MOND acceleration, The modified Newtonian dynamics (MOND) paradigm g (g) = g − g = g − gμ(g/a ). (2) posits that the observations attributed to the presence D N 0 of dark matter can be explained and empirically uni- It seems from the behavior of the interpolating function fied as a modification of Newtonian dynamics when the as dictated by Milgrom’s formula (Brada & Milgrom gravitational acceleration falls below a constant value 1999) that the acceleration equation (2) is universally −10 −2 of a0 10 ms . -
The Standard Model and Beyond Maxim Perelstein, LEPP/Cornell U
The Standard Model and Beyond Maxim Perelstein, LEPP/Cornell U. NYSS APS/AAPT Conference, April 19, 2008 The basic question of particle physics: What is the world made of? What is the smallest indivisible building block of matter? Is there such a thing? In the 20th century, we made tremendous progress in observing smaller and smaller objects Today’s accelerators allow us to study matter on length scales as short as 10^(-18) m The world’s largest particle accelerator/collider: the Tevatron (located at Fermilab in suburban Chicago) 4 miles long, accelerates protons and antiprotons to 99.9999% of speed of light and collides them head-on, 2 The CDF million collisions/sec. detector The control room Particle Collider is a Giant Microscope! • Optics: diffraction limit, ∆min ≈ λ • Quantum mechanics: particles waves, λ ≈ h¯/p • Higher energies shorter distances: ∆ ∼ 10−13 cm M c2 ∼ 1 GeV • Nucleus: proton mass p • Colliders today: E ∼ 100 GeV ∆ ∼ 10−16 cm • Colliders in near future: E ∼ 1000 GeV ∼ 1 TeV ∆ ∼ 10−17 cm Particle Colliders Can Create New Particles! • All naturally occuring matter consists of particles of just a few types: protons, neutrons, electrons, photons, neutrinos • Most other known particles are highly unstable (lifetimes << 1 sec) do not occur naturally In Special Relativity, energy and momentum are conserved, • 2 but mass is not: energy-mass transfer is possible! E = mc • So, a collision of 2 protons moving relativistically can result in production of particles that are much heavier than the protons, “made out of” their kinetic -
Axion Dark Matter from Higgs Inflation with an Intermediate H∗
Axion dark matter from Higgs inflation with an intermediate H∗ Tommi Tenkanena and Luca Visinellib;c;d aDepartment of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA bDepartment of Physics and Astronomy, Uppsala University, L¨agerhyddsv¨agen1, 75120 Uppsala, Sweden cNordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, 10691 Stockholm, Sweden dGravitation Astroparticle Physics Amsterdam (GRAPPA), Institute for Theoretical Physics Amsterdam and Delta Institute for Theoretical Physics, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands E-mail: [email protected], [email protected], [email protected] Abstract. In order to accommodate the QCD axion as the dark matter (DM) in a model in which the Peccei-Quinn (PQ) symmetry is broken before the end of inflation, a relatively low scale of inflation has to be invoked in order to avoid bounds from DM isocurvature 9 fluctuations, H∗ . O(10 ) GeV. We construct a simple model in which the Standard Model Higgs field is non-minimally coupled to Palatini gravity and acts as the inflaton, leading to a 8 scale of inflation H∗ ∼ 10 GeV. When the energy scale at which the PQ symmetry breaks is much larger than the scale of inflation, we find that in this scenario the required axion mass for which the axion constitutes all DM is m0 . 0:05 µeV for a quartic Higgs self-coupling 14 λφ = 0:1, which correspond to the PQ breaking scale vσ & 10 GeV and tensor-to-scalar ratio r ∼ 10−12. Future experiments sensitive to the relevant QCD axion mass scale can therefore shed light on the physics of the Universe before the end of inflation.