DOCSLIB.ORG

UNIVERSITY of CALIFORNIA Los Angeles Exotic

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
UNIVERSITY of CALIFORNIA Los Angeles Exotic UNIVERSITY OF CALIFORNIA Los Angeles Exotic Dark Matter Candidates Generated from Scalar Field Condensation in the Early Universe A dissertation submitted in partial satisfaction of the requirements for the degree Doctor of Philosophy in Physics by Eric Welch Cotner 2018 c Copyright by Eric Welch Cotner 2018 ABSTRACT OF THE DISSERTATION Exotic Dark Matter Candidates Generated from Scalar Field Condensation in the Early Universe by Eric Welch Cotner Doctor of Philosophy in Physics University of California, Los Angeles, 2018 Professor Alexander Kusenko, Chair Scalar fields, though simple conceptually and mathematically, can be responsible for a wide array of emergent phenomena, such as spontaneous symmetry breaking, superconductivity, and the production of solitons. These fields may be responsible for the creation of, or even the identity of, dark matter. This manuscript details the production of dark matter from scalar fields in the form of Q-balls, boson stars, and primordial black holes, and explores the consequences of the existence of such objects and their interactions. ii The dissertation of Eric Welch Cotner is approved. E T Tomboulis Roberto Peccei Graciela B Gelmini Alexander Kusenko, Committee Chair University of California, Los Angeles 2018 iii To my mother, who I hope would have been very proud. To my father, who somehow managed to bring me up right. To my cats, for their unwavering support and insightful discussions. iv TABLE OF CONTENTS 1 Background :::::::::::::::::::::::::::::::::::::: 1 1.1 History . .1 1.2 Exotic Dark Matter Candidates . .3 1.2.1 Q-balls . .3 1.2.2 Boson Stars . .5 1.2.3 Primordial Black Holes . .6 2 Boson Star Collisions :::::::::::::::::::::::::::::::: 7 2.1 Introduction . .7 2.2 Existence and stability of boson stars in the non-relativistic limit . .9 2.3 Binary interactions . 15 2.4 Numerical Simulation . 23 2.4.1 N1 = N2, ξ 1, α = 0, v0 = 0 ...................... 26 2.4.2 N1 = N2, ξ 1, α = 0, v0 = 0 ...................... 27 6 2.4.3 N1 = N2, ξ 1, α = π, v0 = 0 ...................... 27 2.4.4 N1 = N2, ξ 1, α = π, v0 = 0 ...................... 28 2.4.5 N1 N2, ξ 1, α = π, v0 = 0 ..................... 29 2.4.6 N1 N2, ξ 1, α = 0, v0 = 0 ..................... 29 2.4.7 Behavior of unstable soliton with ξ < 1 ................ 30 − 2.5 Discussion . 31 2.5.1 Results of this paper . 31 2.5.2 Implications for dark matter . 34 2.6 Conclusion . 35 v 2.7 Acknowledgment . 35 3 Infection of Neutron Stars by Baryonic Q-balls :::::::::::::::: 36 3.1 Introduction . 36 3.2 Stable Q-ball states . 38 3.2.1 Flat direction Q-balls . 39 3.2.2 Curved direction Q-balls . 40 3.3 The decay rate . 41 3.3.1 Mathematical background . 42 3.3.2 Mass eigenstates and phonons . 44 3.3.3 Calculation of the matrix element . 45 3.3.4 Calculation of the decay rate . 49 3.4 Interactions between Q-balls and neutron stars . 52 3.4.1 Surface conversion of neutron flux . 53 3.4.2 Hydrodynamic considerations due to pion production . 53 3.5 Baryon number evolution in an infected neutron star . 54 3.6 Limits on baryon-violating (and conserving) operators . 56 3.6.1 From decay of Q-balls in free space . 57 3.6.2 From lifetime of neutron stars . 58 3.7 Conclusion . 59 3.8 Acknowledgements . 61 3.9 Appendix: Tables of Q-ball and neutron star lifetimes . 61 4 Primordial Black Holes from Q-ball Clustering :::::::::::::::: 63 4.1 Introduction . 63 4.2 Formation of Q-balls . 65 vi 4.3 Q-ball charge/mass distributions . 66 4.3.1 Single length scale . 68 4.3.2 Multiple length scales . 69 4.4 Q-ball and PBH densities . 71 4.4.1 Q-ball density at fragmentation . 71 4.4.2 Q-ball density perturbations due to fluctuations . 71 4.4.3 Primordial black hole density . 73 4.4.4 Black hole mass spectrum . 75 4.5 Cosmological history . 77 4.5.1 Initial radiation dominated era . 78 4.5.2 Q-ball dominated era . 78 4.5.3 Standard cosmological era . 79 4.6 Observational constraints . 80 4.7 Parameter space . 82 4.8 Topological defects . 84 4.9 Discussion . 85 4.10 Conclusion . 88 4.11 Acknowledgements . 89 4.12 Appendix: Evolution of energy densities . 89 4.12.1 Radiation . 89 4.12.2 Q-balls . 90 4.12.3 Black holes . 90 5 Primordial Black Holes from Inflaton Fragmentation into Oscillons ::: 92 5.1 Introduction . 92 vii 5.2 Oscillons . 93 5.3 Parametric Resonance . 94 5.4 Density Perturbations . 96 5.5 Formation of black holes . 98 5.6 Evolution to present day . 99 5.7 Reheating . 100 5.8 Acknowledgments . 101 References ::::::::::::::::::::::::::::::::::::::::: 102 viii LIST OF FIGURES 1.1 Schematic diagram of the theory space of dark matter. .2 2.1 Boson star total kinetic energy as a function of scaled separation distance x = d=`. 17 2.2 Boson star self-interaction energy as a function of scaled separation distance x = d=`........................................... 18 2.3 Boson star gravitational energy as a function of scaled separation distance x = d=`. 21 2.4 Effective potential (total energy) as a function of scaled separation distance x = d=`. 22 60 −2 2.5 Snapshots of two colliding boson stars with N1 = N2 = 10 , ξ1 = ξ2 = 10 , α = 0 and v0 = 0 ................................... 26 60 −2 2.6 Snapshots of two colliding boson stars with N1 = N2 = 10 , ξ1 = ξ2 = 10 , −15 α = 0 and v0 = 7 10 ............................... 27 × 60 −2 2.7 Snapshots of two colliding boson stars with N1 = N2 = 10 , ξ1 = ξ2 = 10 , α = π, and v0 = 0 ................................... 28 60 1 2.8 Snapshots of two colliding boson stars with N1 = N2 = 10 , ξ1 = ξ2 = 10 , α = π, v0 = 0 ..................................... 28 60 2 −2 2.9 Snapshots of two colliding boson stars with N1 = 10N2 = 10 , ξ1 = 10 ξ2 = 10 , α = π, v0 = 0 ..................................... 29 60 2 1 2.10 Snapshots of two colliding boson stars with N1 = 4N2 = 10 , ξ1 = 4 ξ2 = 10 , α = 0, v0 = 0 ..................................... 30 2.11 Collapse and evolution of an unstable soliton with N = 1060 and ξ = 10 .... 30 − 2.12 Collapse of unstable soliton with small perturbations filtered out . 31 3.1 Schematic scalar potential with a flat direction which is lifted by higher-dimension terms near φ Λ................................... 40 j j ∼ 3.2 Feynman diagram representation of the matrix element responsible for decay of the Q-ball into phonons. 46 ix 3.3 Evolution of charge within the Q-ball at the center of a neutron star . 55 3.4 Charge Q contained within a Q-ball and the number of neutrons consumed by the Q-ball over the life of the neutron star . 56 3.5 Plot of Q-ball lifetimes in free space . 57 3.6 Plot of neutron star lifetimes after being infected by a Q-ball . 58 3.7 Plot of neutron star lifetimes after being infected by a Q-ball (very high dimension operators) . 60 4.1 Schematic illustration of 4 histograms each containing 100 samples from the same Poisson distribution (λ = 100)............................ 67 4.2 Fraction of Q-ball energy that goes into black holes . 74 4.3 Differential PBH/Q-ball density ratio as a function of η = M=Mf ........ 76 4.4 Evolution of energy density over cosmological history . 77 4.5 Comparison of observational PBH constraints fcon(M) = ΩPBH(M)=ΩDM with the dark matter fraction per logarithmic interval . 81 4.6 Parameter space available to PBH production model . 83 5.1 Fraction of super-critical overdensities as a function of the scale factor a(t) ... 95 5.2 DM fraction in primordial black holes. Evolution of cosmological density for parameters of Model A. 97 x LIST OF TABLES 3.1 Table of Q-ball lifetimes (in years) for various lifting potentials . 61 3.2 Table of infected neutron star lifetimes (in years) for various lifting potentials . 62 5.1 Parameter sets for three different PBH production scenarios. 98 xi VITA 2010-2011 Engineering intern with Kyocera America’s Research and Development di- vision. Developed etching procedures for SEM microscopy of solder grain boundaries. 2011-2013 Engineering intern with General Atomcs’ Inertial Fusion Technology divi- sion. Developed fuel injection method for NIF indirect-drive fusion utilizing inductive acceleration and steering of laser targets. 2013 B.S. in Physics, with a minor in Mathematics, UCSD. 2013-2018 Teaching Assistant, Physics and Astronomy Department, UCLA. Taught a variety of discussion and lab sections. Subjects included classical mechan- ics, electrodynamics, quantum mechanics, hydrodynamics, special relativ- ity, particle physics, cosmology. 2014 M.S. in Physics, UCLA. 2014-2018 Research Assistant, Physics and Astronomy Department, UCLA. Studied dark matter, particle astrophysics and cosmology under the supervision of thesis advisor Alexander Kusenko. PUBLICATIONS Primordial Black Holes from Inflaton Fragmentation into Oscillons, E. Cotner, A. Kusenko and V. Takhistov, arXiv:1801.03321 (2018) Primordial black holes from scalar field evolution in the early universe, E. Cotner and A. Kusenko, Phys. Rev. D 96, no. 10, 103002 (2017) xii Primordial black holes from supersymmetry in the early universe, Phys. Rev. Lett. 119, no. 3, 031103 (2017) Astrophysical constraints on dark-matter Q-balls in the presence of baryon-violating opera- tors, E. Cotner and A. Kusenko, Phys. Rev. D 94, no. 12, 123006 (2016) Collisional interactions between self-interacting nonrelativistic boson stars: Effective poten- tial analysis and numerical simulations, E. Cotner, Phys. Rev. D 94, no. 6, 063503 (2016) xiii CHAPTER 1 Background 1.1 History One of the most intriguing scientific questions of our time is the identity of “dark matter", a mysterious substance that pervades the universe.
Load more

Recommended publications
  • Letter of Interest Cosmic Probes of Ultra-Light Axion Dark Matter
    Snowmass2021 - Letter of Interest Cosmic probes of ultra-light axion dark matter Thematic Areas: (check all that apply /) (CF1) Dark Matter: Particle Like (CF2) Dark Matter: Wavelike (CF3) Dark Matter: Cosmic Probes (CF4) Dark Energy and Cosmic Acceleration: The Modern Universe (CF5) Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before (CF6) Dark Energy and Cosmic Acceleration: Complementarity of Probes and New Facilities (CF7) Cosmic Probes of Fundamental Physics (TF09) Astro-particle physics and cosmology Contact Information: Name (Institution) [email]: Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Institute, University of Toronto) [ [email protected]] Authors: Simeon Bird (UC Riverside), Simon Birrer (Stanford University), Djuna Croon (TRIUMF), Alex Drlica-Wagner (Fermilab, University of Chicago), Jeff A. Dror (UC Berkeley, Lawrence Berkeley National Laboratory), Daniel Grin (Haverford College), David J. E. Marsh (Georg-August University Goettingen), Philip Mocz (Princeton), Ethan Nadler (Stanford), Chanda Prescod-Weinstein (University of New Hamp- shire), Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Insti- tute, University of Toronto), Katelin Schutz (MIT), Neelima Sehgal (Stony Brook University), Yu-Dai Tsai (Fermilab), Tien-Tien Yu (University of Oregon), Yimin Zhong (University of Chicago). Abstract: Ultra-light axions are a compelling dark matter candidate, motivated by the string axiverse, the strong CP problem in QCD, and possible tensions in the CDM model. They are hard to probe experimentally, and so cosmological/astrophysical observations are very sensitive to the distinctive gravitational phenomena of ULA dark matter. There is the prospect of probing fifteen orders of magnitude in mass, often down to sub-percent contributions to the DM in the next ten to twenty years.
    [Show full text]
  • Ultra Light Axionic Dark Matter: Galactic Halos and Implications for Observations with Pulsar Timing Arrays
    galaxies Article Ultra Light Axionic Dark Matter: Galactic Halos and Implications for Observations with Pulsar Timing Arrays Ivan de Martino 1,* ID , Tom Broadhurst 1,2, S.-H. Henry Tye 3, Tzihong Chiueh 4, Hsi-Yu Schive 5 and Ruth Lazkoz 1 1 Department of Theoretical Physics, University of the Basque Country UPV/EHU, E-48080 Bilbao, Spain; [email protected] (T.B.); [email protected] (R.L.) 2 Ikerbasque, Basque Foundation for Science, E-48011 Bilbao, Spain 3 Institute for Advanced Study and Department of Physics, Hong Kong University of Science and Technology, Hong Kong, China; [email protected] 4 National Center for Theoretical Sciences, National Taiwan University, Taipei 10617, Taiwan; [email protected] 5 National Center for Supercomputing Applications, Urbana, IL 61801, USA; [email protected] * Correspondence: [email protected] Received: 29 November 2017; Accepted: 8 January 2018; Published: 16 January 2018 Abstract: The cold dark matter (CDM) paradigm successfully explains the cosmic structure over an enormous span of redshifts. However, it fails when probing the innermost regions of dark matter halos and the properties of the Milky Way’s dwarf galaxy satellites. Moreover, the lack of experimental detection of Weakly Interacting Massive Particle (WIMP) favors alternative candidates such as light axionic dark matter that naturally arise in string theory. Cosmological N-body simulations have shown that axionic dark matter forms a solitonic core of size of '150 pc in the innermost region of the galactic halos. The oscillating scalar field associated to the axionic dark matter halo produces an oscillating gravitational potential that induces a time dilation of the pulse arrival time of −22 '400 ns/(mB/10 eV) for pulsar within such a solitonic core.
    [Show full text]
  • The Higgs Boson and the Cosmology of the Early Universe Mikhail Shaposhnikov Blois 2018
    The Higgs Boson and the Cosmology of the Early Universe Mikhail Shaposhnikov Blois 2018 Rencontres de Blois, June 4, 2018 – p. 1 Almost 6 years with the Higgs boson: July 4, 2012, Higgs at ATLAS and CMS 3500 ATLAS Data Sig+Bkg Fit (m =126.5 GeV) 3000 H Bkg (4th order polynomial) 2500 Events / 2 GeV 2000 1500 s=7 TeV, ∫Ldt=4.8fb-1 1000 s=8 TeV, ∫Ldt=5.9fb-1 γγ→ 500 H (a) 200100 110 120 130 140 150 160 100 0 -100 Events - Bkg (b) -200 100 110 120 130 140 150 160 Data S/B Weighted 100 Sig+Bkg Fit (m =126.5 GeV) H Bkg (4th order polynomial) 80 weights / 2 GeV Σ 60 40 20 (c) 8100 110 120 130 140 150 160 4 0 -4 (d) -8 Σ weights - Bkg 100 110 120 130 140 150 160 m γγ [GeV] Rencontres de Blois, June 4, 2018 – p. 2 What did we learn from the Higgs discovery for particle physics? Rencontres de Blois, June 4, 2018 – p. 3 The ideas of the authors of the BEH mechanism were right Rencontres de Blois, June 4, 2018 – p. 4 The Standard Model is now complete Rencontres de Blois, June 4, 2018 – p. 5 126 125 U U U GeV Triumph of the SM in particle physics No significant deviations from the SM have been observed Rencontres de Blois, June 4, 2018 – p. 6 126 125 U U U GeV Triumph of the SM in particle physics No significant deviations from the SM have been observed The masses of the top quark and of the Higgs boson, the Nature has chosen, make the SM a self-consistent effective field theory all the way up to the quantum gravity Planck scale MP .
    [Show full text]
  • Arxiv:1906.00969V2 [Hep-Ph] 2 Sep 2019
    FTUAM-19-11; IFT-UAM/CSIC-19-74 Very Light Asymmetric Dark Matter Gonzalo Alonso-Alvarez´ 1, Julia Gehrlein2;3, Joerg Jaeckel1 and Sebastian Schenk1 1Institut f¨urTheoretische Physik, Universit¨atHeidelberg, Philosophenweg 16, 69120 Heidelberg, Germany 2Instituto de F´ısica Te´orica UAM/CSIC, Calle Nicol´as Cabrera 13-15, Cantoblanco E-28049 Madrid, Spain 3Departamento de F´ısica Te´orica, Universidad Aut´onomade Madrid, Cantoblanco E-28049 Madrid, Spain Abstract Very light dark matter is usually taken to consist of uncharged bosons such as axion-like particles or dark photons. Here, we consider the prospect of very light, possibly even sub- eV dark matter carrying a net charge that is (approximately) conserved. By making use of the Affleck-Dine mechanism for its production, we show that a sizable fraction of the energy density can be stored in the asymmetric component. We furthermore argue that there exist regions of parameter space where the energy density contained in symmetric particle-antiparticle pairs without net charge can to some degree be depleted by considering couplings to additional fields. Finally, we make an initial foray into the phenomenology of this scenario by considering the possibility that dark matter is coupled to the visible sector via the Higgs portal. arXiv:1906.00969v2 [hep-ph] 2 Sep 2019 1 1 Introduction Very light bosons such as axion(-like) particles or dark photons are increasingly popular dark matter candidates (see, e.g., [1,2] for reviews). Currently, a significant and growing experimental community is set to hunt down these very weakly interacting particles [1,3{17].
    [Show full text]
  • The Grand Battle
    the grand battle Alexander Kartavtsev 23 July 2013 23 July 2013 Alexander Kartavtsev 1 Angels and demons Outline 1. Experimental observations 2. Theoretical advancements 3. Electroweak baryogenesis 4. Baryogenesis via leptogenesis 5. Current status 6. Summary 23 July 2013 Alexander Kartavtsev 3 Antimatter predicted (1928) … during his postgraduate years he concentrated solely on his research, and stopped only on Sunday, when he took long strolls alone … Paul Dirac 23 July 2013 Alexander Kartavtsev 5 Antimatter discovered (1932) Carl Anderson 23 July 2013 Alexander Kartavtsev 7 Cosmic rays (1936) Homi Bhabha 23 July 2013 Alexander Kartavtsev 8 Cosmic rays contain positrons and antiprotons 23 July 2013 Alexander Kartavtsev 9 Cosmic rays would contain complex antiatoms 23 July 2013 Alexander Kartavtsev 10 23 July 2013 Alexander Kartavtsev 11 CMB (1965) Robert Woodrow Wilson Arno Allan Penzias 23 July 2013 Alexander Kartavtsev 13 Baryon to photon ratio = 6.1x10-10 23 July 2013 Alexander Kartavtsev 14 23 July 2013 Alexander Kartavtsev 15 BBN η = 5.8x10-10 23 July 2013 Alexander Kartavtsev 16 Inflation Alan Guth 23 July 2013 Alexander Kartavtsev 17 Generation of the baryon asymmetry 23 July 2013 Alexander Kartavtsev 18 Sakharov conditions (1967) Violation of baryon number C- and CP-violation Deviation from equilibrium Andrei Sakharov 23 July 2013 Alexander Kartavtsev 19 Standard model (1967) Sheldon Glashow Steven Weinberg Abdus Salam 23 July 2013 Alexander Kartavtsev 20 Baryon number violation ? 23 July 2013 Alexander Kartavtsev 21 Dirac sea 23 July 2013 Alexander Kartavtsev 23 Dirac sea 23 July 2013 Alexander Kartavtsev 24 Sphalerons (1984) Frans Klinkhamer Nick Manton 23 July 2013 Alexander Kartavtsev 26 CP-violation James Cronin Val Fitch 23 July 2013 Alexander Kartavtsev 27 Deviation from equilibrium 23 July 2013 Alexander Kartavtsev 28 First order transition ? 23 July 2013 Alexander Kartavtsev 29 Electroweak baryogenesis (1985) Valery Rubakov Vadim Kuzmin Mikhail Shaposhnikov 23 July 2013 Alexander Kartavtsev 30 B-L = const.
    [Show full text]
  • TITLES and ABSTRACTS First Name: Andrea Surname: Addazi
    TITLES AND ABSTRACTS First Name: Andrea Surname: Addazi Affiliation: Fudan University (Shanghai) Quantum Vacuum & Quantum black holes: two aspects of the same question ---------------------------------------------------------------------------------------- Quantum vacuum and Quantum black holes may be considered as two aspects of the same problem. First of all, we will show how virtual black hole pairs provide a planckian contribution to the vacuum energy which screens the contribution coming from Standard Model vacuum energy. Second, we will move on the possible relation of dark energy and (Anti)evaporation instabilities in the framework of f(R)-gravity, In this case, a model for cosmology may provide insightful intuitions on the black hole thermodynamics and the information paradox. First Name: Imanol Surname: Albarran Affiliation: Universidade da Beira Interior The quantum realm of the "Little Sibling" of the Big Rip singularity ---------------------------------------------------------------------------------------- We analyse the quantum behaviour of the Little Sibling of the Big Rip singularity (LSBR). The quantisation is carried within the geometrodynamical approach given by the Wheeler- DeWitt(WDW)equation. The classical model is based on a Friedmann-Lemaître- Robertson-Walker Universe filled by a perfect fluid that can be mapped to a scalar field with phantom character. We analyse the WDW equation in two setups. In the fi rst step, we consider the scale factor as the single degree of freedom, which from a classical perspective parametrises both the geometry and the matter content given by the perfect fluid. We then solve the WDW equation within a WKB approximation, for two factor ordering choices. On the second approach, we consider the WD equation with two degrees of freedom: the scale factor and a scalar fi eld.
    [Show full text]
  • Cosmology Meets Condensed Matter
    Cosmology Meets Condensed Matter Mark N. Brook Thesis submitted to the University of Nottingham for the degree of Doctor of Philosophy. July 2010 The Feynman Problem-Solving Algorithm: 1. Write down the problem 2. Think very hard 3. Write down the answer – R. P. Feynman att. to M. Gell-Mann Supervisor: Prof. Peter Coles Examiners: Prof. Ed Copeland Prof. Ray Rivers Abstract This thesis is concerned with the interface of cosmology and condensed matter. Although at either end of the scale spectrum, the two disciplines have more in common than one might think. Condensed matter theorists and high-energy field theorists study, usually independently, phenomena embedded in the structure of a quantum field theory. It would appear at first glance that these phenomena are disjoint, and this has often led to the two fields developing their own procedures and strategies, and adopting their own nomenclature. We will look at some concepts that have helped bridge the gap between the two sub- jects, enabling progress in both, before incorporating condensed matter techniques to our own cosmological model. By considering ideas from cosmological high-energy field theory, we then critically examine other models of astrophysical condensed mat- ter phenomena. In Chapter 1, we introduce the current cosmological paradigm, and present a somewhat historical overview of the interplay between cosmology and condensed matter. Many concepts are introduced here that later chapters will follow up on, and we give some examples in which condensed matter physics has had a very real effect on informing cosmology. We also reflect on the most recent incarnations of the condensed matter / cosmology interplay, and the future of these developments.
    [Show full text]
  • Scale Invariant Models for BSM Physics and Cosmology Mikhail Shaposhnikov
    Scale invariant models for BSM physics and cosmology Mikhail Shaposhnikov SUSY: Model-building and Phenomenology IPMU, 4 December 2013 Tokyo, 4 December 2013 – p. 1 M.S., Daniel Zenhäusern, Phys. Lett. B 671 (2009) 162 M.S., Daniel Zenhäusern, Phys. Lett. B 671 (2009) 187 F. Tkachov, M.S., arXiv:0905.4857 Diego Blas, M.S., Daniel Zenhäusern, Phys. Rev. D84 (2011) 044001 Juan García-Bellido, Javier Rubio, M.S., Daniel Zenhäusern, Phys. Rev. D84 (2011) 123504 F. Bezrukov, M. Kalmykov, B. Kniehl, M.S. JHEP 1210(2012) 140 Juan García-Bellido, Javier Rubio, M.S., Phys. Lett. (2012) F. Bezrukov, G. K. Karananas, J. Rubio and M.S., Phys. Rev. D 87, 096001 (2013) R. Armillis, A. Monin and M.S., JHEP 1310, 030 (2013) A. Monin and M. S., Phys. Rev. D 88, 067701 (2013) Tokyo, 4 December 2013 – p. 2 Outline The proposal in short Diff versus TDiff Field theory: classical scale invariance and its spontaneous breakdown Unimodular gravity Scale invariance, unimodular gravity, cosmological constant, inflation and dark energy Quantum scale invariance Dilaton as a part of the metric in TDiff gravity Conclusions Tokyo, 4 December 2013 – p. 3 An alternative to SUSY, large extra dimensions, technicolor, etc Effective Theory Of Everything Tokyo, 4 December 2013 – p. 4 An alternative to SUSY, large extra dimensions, technicolor, etc Effective Theory Of Everything Tokyo, 4 December 2013 – p. 5 Definitions “Effective”: valid up to the Planck scale, quantum gravity problem is not addressed. No new particles heavier than the Higgs boson. “Everything”: neutrino masses and oscillations dark matter baryon asymmetry of the Universe inflation dark energy Tokyo, 4 December 2013 – p.
    [Show full text]
  • Standard Model Meets Gravity: Electroweak Symmetry Breaking and Inflation
    PHYSICAL REVIEW D 103, 033006 (2021) Standard model meets gravity: Electroweak symmetry breaking and inflation † ‡ Mikhail Shaposhnikov ,* Andrey Shkerin , and Sebastian Zell Institute of Physics, Laboratory for Particle Physics and Cosmology, École Polytechnique F´ed´erale de Lausanne, CH-1015 Lausanne, Switzerland (Received 19 February 2020; revised 23 November 2020; accepted 2 February 2021; published 25 February 2021) We propose a model for combining the Standard Model (SM) with gravity. It relies on a nonminimal coupling of the Higgs field to the Ricci scalar and on the Palatini formulation of gravity. Without introducing any new degrees of freedom in addition to those of the SM and the graviton, this scenario achieves two goals. First, it generates the electroweak symmetry breaking by a nonperturbative gravitational effect. In this way, it does not only address the hierarchy problem but opens up the possibility to calculate the Higgs mass. Second, the model incorporates inflation at energies below the onset of strong-coupling of the theory. Provided that corrections due to new physics above the scale of inflation are not unnaturally large, we can relate inflationary parameters to data from collider experiments. DOI: 10.1103/PhysRevD.103.033006 I. INTRODUCTION Other experimental and observational data that calls for The results of LHC have been very exciting. First, it has new physics, such as dark matter, neutrino oscillations and found the last missing particle of the Standard Model (SM), baryon asymmetry of the Universe, does not require the presence of any new particle populating the desert between the Higgs boson [1,2]. Second, it has significantly con- 2 strained physics beyond the SM.
    [Show full text]
  • Kobe University Repository : Kernel
    Kobe University Repository : Kernel タイトル Pulsar timing residual induced by ultralight vector dark matter Title 著者 Nomura, Kimihiro / Ito, Asuka / Soda, Jiro Author(s) 掲載誌・巻号・ページ European Physical Journal C,80(5):419 Citation 刊行日 2020-05-14 Issue date 資源タイプ Journal Article / 学術雑誌論文 Resource Type 版区分 publisher Resource Version © The Author(s) 2020. This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party 権利 material in this article are included in the article’s Creative Commons Rights licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/. Funded by SCOAP3 DOI 10.1140/epjc/s10052-020-7990-y JaLCDOI URL http://www.lib.kobe-u.ac.jp/handle_kernel/90007118 PDF issue: 2021-09-30 Eur. Phys. J. C (2020) 80:419 https://doi.org/10.1140/epjc/s10052-020-7990-y Regular Article - Theoretical Physics Pulsar timing residual induced by ultralight vector dark matter Kimihiro Nomuraa, Asuka Itob, Jiro Sodac Department of Physics, Kobe University, Kobe 657-8501, Japan Received: 12 March 2020 / Accepted: 28 April 2020 © The Author(s) 2020 Abstract We study the ultralight vector dark matter with for a free field to condense homogeneously during inflation.
    [Show full text]
  • Arxiv:1703.03286V1 [Gr-Qc] 7 Mar 2017 They Have a finite Size and Density Profile, Which Leads to an Effective Softening Force at Small Scales [16],[17]
    Description of the evolution of inhomogeneities on a Dark Matter halo with the Vlasov equation Paola Domínguez-Fernández,1, ∗ Erik Jiménez-Vázquez,2, y Miguel Alcubierre,2, z Edison Montoya,3, x and Darío Núñez2, { 1Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121, Bonn, Germany 2Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Circuito Exterior C.U., A.P. 70-543, México D.F. 04510, México 3Escuela de Física, Universidad Industrial de Santander, A.A. 678, Bucaramanga, Colombia (Dated: May 15, 2018) We use a direct numerical integration of the Vlasov equation in spherical symmetry with a back- ground gravitational potential to determine the evolution of a collection of particles in different models of a galactic halo. Such a collection is assumed to represent a dark matter inhomogeneity which reaches a stationary state determined by the virialization of the system. We describe some features of the stationary states and, by using several halo models, obtain distinctive signatures for the evolution of the inhomogeneities in each of the models. PACS numbers: 11.15.Bt, 04.30.-w, 95.30.Sf I. INTRODUCTION The nature of dark matter remains one of the most puzzling questions in modern cosmology. Its assumed that elementary particles could be the constituents of dark matter for which there have been several experimental attempts to perform a direct detection of such dark matter particle, but still a clear evidence for such particles remains absent [1]. Examples of these experiments are the Large Underground Xenon (LUX) experiment [2], the DAMA/Libra experiment [3], ZEPLIN experiment [4], XENON10 experiment [5] or DAMIC experiment at SNOLAB [6], [7–9].
    [Show full text]
  • Techniques for Inelastic Effective Field Theory Measurements with the Large Underground Xenon Experiment by Daniel Patrick Hogan
    Techniques for Inelastic Effective Field Theory Measurements with the Large Underground Xenon Experiment by Daniel Patrick Hogan A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Robert Jacobsen, Chair Professor Marjorie Shapiro Professor Kai Vetter Summer 2018 Techniques for Inelastic Effective Field Theory Measurements with the Large Underground Xenon Experiment Copyright 2018 by Daniel Patrick Hogan 1 Abstract Techniques for Inelastic Effective Field Theory Measurements with the Large Underground Xenon Experiment by Daniel Patrick Hogan Doctor of Philosophy in Physics University of California, Berkeley Professor Robert Jacobsen, Chair Cosmological evidence indicates that nonbaryonic dark matter makes up a quarter of the energy density of the universe. One hypothesis for the particle nature of dark matter is the weakly-interacting massive particle (WIMP). The Large Underground Xenon (LUX) experiment is a dual-phase xenon WIMP search experiment with a 250kg active volume. Computational tools developed to support LUX analyses include data mirroring and a data visualization web portal. Within the LUX detector, particle interactions produce pulses of scintillation light. A pulse shape discrimination (PSD) technique is shown to help classify interaction events into nuclear recoils and electron recoils based on the time-structure of the pulses. This approach is evaluated in the context of setting limits on inelastic effective field theory (IEFT) dark matter models. Although PSD is not found to provide significant improvement in the limits, LUX is nevertheless able to set world-leading limits on some IEFT models, while limits for other IEFT models are reported here for the first time.
    [Show full text]