DOCSLIB.ORG

Recent Topics in Axion Cosmology -Isocurvature Perturbations and Alignment

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Recent Topics in Axion Cosmology -Isocurvature Perturbations and Alignment Recent topics in axion cosmology -isocurvature perturbations and alignment- 30th June 2016 seminar@Osaka U. Fuminobu Takahashi (Tohoku) Kawasaki, FT, Yamada, 1511.05030 Higaki, Jeong, Kitajima, FT, 1512.05295, 1603.02090, Higaki, Jeong, Kitajima, Sekiguchi, FT, 1606.05552 The Strong CP Problem g2 = ✓ s Gaµ⌫ G˜a L✓ 32⇡2 µ⌫ Experimental bound from neutron electric dipole moment reads 10 ✓ < 10− | | Why is ✓ so small is the strong CP problem. cf. More precisely, the physical strong CP phase is ✓¯ ✓ arg det (M M ) ⌘ − u d which makes the problem even more puzzling. A plausible solution is the Peccei-Quinn mechanism where the CP phase is promoted to a dynamical variable: Peccei, Quinn `77, Weinberg `78, Wilczek `78 a g2 = ✓ + s Gaµ⌫ G˜a L✓ f 32⇡2 µ⌫ ✓ a ◆ T Λ QCD T ΛQCD a The QCD axion dynamically cancels the stronga CP phase. Accordingly, the axion DM is produced as coherent oscillations [misalignment mechanism]. f 1.19 ⇤ ⌦ h2 =0.18 ✓2 a QCD a i 1012 GeV 400 MeV ✓ ◆ ✓ ◆ If the axion exists during inflation, it acquires isocurvature fluctuations. δ⌦ ✓ a =2 i ⌦a ✓i δa = Hinf /2π T Λ QCD T Λ QCD a a Axion isocurvature perturbations Adiabatic perturbation Isocurvature perturbation ρ ρ photon photon DM/baryon DM/baryon x x ⌦ δ⌦ ⌦ 2✓ ⌦ H S = a a = a i = a inf ⌦CDM ⌦a ⌦CDM ✓i ⌦CDM ⇡✓ifa S Planck 2015 βiso = P < 0.038 (95% CL) (Planck TT, TE, EE + lowP) + S PR P CMB angular power spectrum Adiabatic Isocurvature Planck CMB angular power spectrum Adiabatic Isocurvature ⌦ ✓ ⌦ H S =2 a i = a inf ⌦CDM ✓i ⌦CDM ⇡✓ifa (Taken from Kawasaki’s slide) Isocurvature constraint on Hinf r = 0.01 9 10 r = 0.1 108 r = ⌦a/⌦DM 107 r = 1 106 7 8 105 Hinf 10 − GeV 104 GeV / 103 inf 102 Anharmonic H 101 effects 100 - 10 1 - 10 2 - 10 3 109 1010 1011 1012 1013 1014 Kobayashi, Kurematsu, FT, 1304.0922 fa / GeV Axion DM is in severe tension w/ many inflation models! Solutions to isocuvature problem 1)Restoration of Peccei-Quinn symmetry during inflation. Linde and Lyth `90 Lyth and Stewart `92 Figure taken from M. Kawasaki’s slide Solutions to isocuvature problem 1)Restoration of Peccei-Quinn symmetry during inflation. Linde and Lyth `90 Lyth and Stewart `92 • Axions are produced from domain walls and 10 axion DM is possible for fa = 10 GeV. Hiramatsu, Kawasaki, Saikawa and Sekiguchi, 1202.5851,1207.3166 Solutions to isocuvature problem 1)Restoration of Peccei-Quinn symmetry during inflation. Linde and Lyth `90 Lyth and Stewart `92 • Axions are produced from domain walls and 10 axion DM is possible for fa = 10 GeV. Hiramatsu, Kawasaki, Saikawa and Sekiguchi, 1202.5851,1207.3166 2)(Super-)Planckian saxion field value during inflation. (Saxion could be the inflaton) Linde and Lyth `90 Linde, `91 Axion: phase component Saxion: radial component Solutions to isocuvature problem 3)Resonant mixing with another axion. Kitajima, FT 1411.2011 cf. Hill, Ross `88 2 2 4)Heavy axions during inflation ma & Hinf • Stronger QCD during inflation cf. Dvali, `95, Jeong, FT 1304.8131 Choi et al, 1505.00306 • Extra explicit PQ breaking Dine, Anisimov hep-ph/0405256 Higaki, Jeong, FT, 1403.4186, Barr and J.E.Kim, 1407.4311 FT and Yamada 1507.06387 a The extra PQ breaking term must be sufficiently suppressed at present. Solutions to isocuvature problem In the following, I will talk about two solutions and their implications: (1) The Witten effect Explicit PQ breaking (2) Alignment mechanism Restoration of PQ symmetry Witten effect Witten `79 Let us first consider the θ-term of hidden U(1): This θ is not the ✓e2 ✓e2 strong CP phase. = F F˜µ⌫ = E B L✓ 32⇡2 µ⌫ −8⇡2 · which usually has no effect as it is a total derivative. The term, however, has an interesting effect in the monopole background. B B +θ-term Mono Dyon E pole QM =4⇡/e QM =4⇡/e Q =0 E 6 Witten effect Witten `79 Consider a static EM field and a monopole sitting at the origin: due to Coleman Q rˆ E = gradφ = A0 B = A + M − r r⇥ 4⇡ r2 Then, the Lagrangian is Monopole ✓e2 L = d3r E B ✓ −8⇡2 · Z ✓ ◆ ✓e2 Q rˆ = d3r A0 A + M −8⇡2 r · r⇥ 4⇡ r2 Z ✓ ◆ ✓ ◆ ✓e2Q rˆ = d3rA0 M − 8⇡2 r 4⇡r2 Z ✓ ◆ ✓ ◆ ✓e2Q = d3rA0 M δ(3)(r) − 8⇡2 Z ✓ Electric◆ charge at the origin Witten effect Witten `79 A monopole acquires an electric charge, B and becomes a dyon if ✓ =0 . 6 Dyon E e✓ Q = ne + n =0, 1, 2, E 2⇡ ± ± ··· A monopole magnetic charge Q M =4 ⇡ /e is used. QM =4⇡/e Q =0 E 6 The mass of dyons is heavier than the monopole mass: 1 m2 ✓ 2 M = M + W n D M 2 M − 2⇡ M ✓ ◆ v Q2 + Q2 ' M E The non-zero value ofq θ costs more energy as it induces an electric field around the monopole. Axion coupled to hidden monopoles Kawasaki, FT, Yamada, 1511.05030 Consider the axion coupling to U(1)H: 2 2 e a ˜µ⌫ e a ✓ = 2 Fµ⌫ F = 2 E B L 32⇡ fa −8⇡ fa · Then, the QCD axion acquires an extra mass about a =0 by the Witten effect in the presence of hidden monopoles: 2 ↵ nM ma,M 2 2 ' 16⇡ rcfa cf. Fischler and Preskill, `83 e2 nM :(anti-)monopole number density ↵ = 4⇡ 1 1 rc = : monopole radius ' ev mW •The extra axion mass naturally decreases as the monopole density is diluted by the cosmic expansion. Consistent w/ the neutron EDM constraint. Evolution of axion •The axion starts to oscillate when m 2 H 2. a,M ' 2 ⌦ h2 f − T 65 GeV↵2 M a . osc,1 ' 0.12 1012 GeV ✓ ◆✓ ◆ Witten effect a •No extra axion coherent oscillations are induced during the QCD phase transition if m /H (10) . a,M & O ⌦ h2 0.55 f 1012 GeV↵1.1 M . a . 0.12 ✓ ◆ “Adiabatic suppression mechanism” Linde `96. +QCD instanton Witten effect a Axion abundance Kawasaki, FT, Yamada, 1511.05030 The final axion abundance is given by 3 2 4 2 2 0.12 fa ⌦ h 3 10− ↵− ✓ a ' ⇥ i ⌦ h2 1012 GeV ✓ M ◆✓ ◆ The axion abundance is suppressed, and it is inversely proportional to the monopole abundance! The Witten effect also solves the axion domain wall problem when the PQ symmetry spontaneously broken after inflation. QCD axion and monopole DM 0.12 Monopole dominated DM 2 3 2 12 3 0.10 θinifa /α =(4×10 GeV) 0.08 Ω a h 2 + 2 Ω m 2h h ⌦M h 0.06 2 m = 0.12 Ω 0.04 2 3 2 12 3 θinifa /α =(2×10 GeV) Axion dominated 0.02 2 3 2 12 3 θinifa /α =(1×10 GeV) DM 0.00 0.00 0.02 0.04 0.06 0.08 0.10 0.12 2 ⌦ h 2 Kawasaki, FT, Yamada, 1511.05030 Ωaah Hidden monopole DM The monopoles with mass M =(1 10) PeV account for M − the observed DM. Murayama, Shu 0905.1720 In the minimal case of the ’t Hooft-Polyakov monopole w/o other charged particles, the massive gauge bosons give a larger contribution. Baek, Ko, Park 1311.1035, Khoze, Ro 1406.2291 e.g. The observed DM is realized with v 102 TeV, ↵ = (0.1) ' O for which the monopole fraction is O(10)%. N.B. The massive gauge boson abundance can be reduced by adding matter fields. Discussion • The monopoles (as well as W’) have self-interactions which may solve the small-scale tension of CDM. Baek, Ko, Park 1311.1035, Khoze, Ro 1406.2291 • The monopole DM may also have the SM electromagnetic mini-charges via the kinetic mixing: φa µ⌫ (EM) v µ⌫ (EM) Fa Fµ⌫ F3 Fµ⌫ φa =(0, 0,v) M ⊃ M h i 2 13 For v 10 TeV,M Mp the kinetic mixing is 10− ⇠ ⇠ (& magnetic) ⇠ and it is consistent with observations. cf. Jaeckel and Ringwald, 1002.0329 • If U(1)H is broken by another Higgs, monopoles and W’ become unstable and decay into the SM particles via the portal to the SM Higgs. The QCD axion abundance can be suppressed for even larger f a . Kawasaki, FT, Yamada, 1511.05030 cf. Nomura, Rajendran, Sanches, 1511.06347 Aligned QCD axion Higaki, Jeong, Kitajima, FT, 1512.05295, 1603.02090, Higaki, Jeong, Kitajima, Sekiguchi, FT, 1606.05552 No axion isocurvature perturbations if the PQ symmetry is restored during or after inflation. Is high TR or Hinf necessary? Classical axion window: TR,Hinf & Fa 9 12 10 GeV . Fa . 10 GeV Decay constant = PQ breaking scale? In a simple set-up, V (Φ) Φ F h i⇠ a Φ : PQ scalar However, this is not necessarily the case. If there are multiple PQ scalars, Φ F h i⌧ a is possible. Alignment mechanism The decay constant can be enhanced by the largest hierarchy among the PQ charges in the alignment mechanism, See also Sikivie `86 Kim, Nilles, Peloso, hep-ph/0409138 Choi, Kim, Yun, 1404.6209, Higaki, FT, 1404.6923 Harigaya and Ibe, 1407.4893, Choi and Im, 1511.00132, Kaplan and Rattzzi, 1511.01827. Clockwork axion model with N=2: 2 Φ2 Φ V = ( m2 Φ 2 + λ Φ 4) 1 − i | i| i| i| i=1 X 3 + ✏ Φ1Φ2 +h.c. fi + si iai/fi Φi = e p2 2 2 2 3f1a1 f2a2 fa = 3 f1 + f2 ,a= − fa q Alignment with multiple axions Choi, Kim, Yun, 1404.6209, Higaki, FT, 1404.6923 Harigaya and Ibe, 1407.4893, Choi and Im, 1511.00132, Kaplan and Rattzzi, 1511.01827.
Load more

Recommended publications
  • Axions and Other Similar Particles
    1 91. Axions and Other Similar Particles 91. Axions and Other Similar Particles Revised October 2019 by A. Ringwald (DESY, Hamburg), L.J. Rosenberg (U. Washington) and G. Rybka (U. Washington). 91.1 Introduction In this section, we list coupling-strength and mass limits for light neutral scalar or pseudoscalar bosons that couple weakly to normal matter and radiation. Such bosons may arise from the spon- taneous breaking of a global U(1) symmetry, resulting in a massless Nambu-Goldstone (NG) boson. If there is a small explicit symmetry breaking, either already in the Lagrangian or due to quantum effects such as anomalies, the boson acquires a mass and is called a pseudo-NG boson. Typical examples are axions (A0)[1–4] and majorons [5], associated, respectively, with a spontaneously broken Peccei-Quinn and lepton-number symmetry. A common feature of these light bosons φ is that their coupling to Standard-Model particles is suppressed by the energy scale that characterizes the symmetry breaking, i.e., the decay constant f. The interaction Lagrangian is −1 µ L = f J ∂µ φ , (91.1) where J µ is the Noether current of the spontaneously broken global symmetry. If f is very large, these new particles interact very weakly. Detecting them would provide a window to physics far beyond what can be probed at accelerators. Axions are of particular interest because the Peccei-Quinn (PQ) mechanism remains perhaps the most credible scheme to preserve CP-symmetry in QCD. Moreover, the cold dark matter (CDM) of the universe may well consist of axions and they are searched for in dedicated experiments with a realistic chance of discovery.
    [Show full text]
  • Gaugino Mass in Heavy Sfermion Scenario
    IPMU 15-0137 Gaugino mass in heavy sfermion scenario Keisuke Harigaya1, 2 1Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, 277-8583, Japan 2ICRR, University of Tokyo, Kashiwa, Chiba 277-8582, Japan (Dated: May 8, 2018) Abstract The heavy sfermion scenario is naturally realized when supersymmetry breaking fields are charged under some symmetry or are composite fields. There, scalar partners of standard model fermions and the gravitino are as heavy as O(10-1000) TeV while gauginos are as heavy as O(1) TeV. The scenario is not only consistent with the observed higgs mass, but also is free from cosmo- logical problems such as the Polonyi problem and the gravitino problem. In the scenario, gauginos are primary targets of experimental searches. In this thesis, we discuss gaugino masses in the heavy sfermion scenario. First, we derive the so-called anomaly mediated gaugino mass in the superspace formalism of supergravity with a Wilsonian effective action. Then we calculate gaugino masses generated through other possible one-loop corrections by extra light matter fields and the QCD axion. Finally, we consider the case where some gauginos are degenerated in their masses with each other, because the thermal relic abundance of the lightest supersymmetric particle as well as the the strategy to search gauginos drastically change in this case. After calculating the thermal relic abundance of the lightest supersymmetric particle for the degenerated case, we discuss the phenomenology of gauginos at the Large Hadron Collider and cosmic ray experiments. arXiv:1508.04811v1 [hep-ph] 19 Aug 2015 1 Contents I. Introduction 6 II.
    [Show full text]
  • QCD Axion Dark Matter with a Small Decay Constant
    UC Berkeley UC Berkeley Previously Published Works Title QCD Axion Dark Matter with a Small Decay Constant. Permalink https://escholarship.org/uc/item/61f6p95k Journal Physical review letters, 120(21) ISSN 0031-9007 Authors Co, Raymond T Hall, Lawrence J Harigaya, Keisuke Publication Date 2018-05-01 DOI 10.1103/physrevlett.120.211602 Peer reviewed eScholarship.org Powered by the California Digital Library University of California PHYSICAL REVIEW LETTERS 120, 211602 (2018) Editors' Suggestion QCD Axion Dark Matter with a Small Decay Constant Raymond T. Co,1,2,3 Lawrence J. Hall,2,3 and Keisuke Harigaya2,3 1Leinweber Center for Theoretical Physics, University of Michigan, Ann Arbor, Michigan 48109, USA 2Department of Physics, University of California, Berkeley, California 94720, USA 3Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA (Received 20 December 2017; published 23 May 2018) The QCD axion is a good dark matter candidate. The observed dark matter abundance can arise from 11 misalignment or defect mechanisms, which generically require an axion decay constant fa ∼ Oð10 Þ GeV (or higher). We introduce a new cosmological origin for axion dark matter, parametric resonance from 8 11 oscillations of the Peccei-Quinn symmetry breaking field, that requires fa ∼ ð10 –10 Þ GeV. The axions may be warm enough to give deviations from cold dark matter in large scale structure. DOI: 10.1103/PhysRevLett.120.211602 Introduction.—The absence of CP violation from QCD is unstable and decays into axions [10], yielding a dark is a long-standing problem in particle physics [1] and is matter density [11,12] elegantly solved by the Peccei-Quinn (PQ) mechanism 1.19 [2,3] involving a spontaneously broken anomalous sym- 2 fa Ω h j − ≃ 0.04–0.3 : ð2Þ metry.
    [Show full text]
  • Unifying Inflation with the Axion, Dark Matter, Baryogenesis, and the Seesaw Mechanism
    Unifying Inflation with the Axion, Dark Matter, Baryogenesis, and the Seesaw Mechanism. Andreas Ringwald Astroteilchenseminar Max-Planck-Institut für Kernphysik Heidelberg, D 13 November 2017 [Guillermo Ballesteros, Javier Redondo, AR, Carlos Tamarit, 1608.05414; 1610.01639] Fundamental Problems > Standard Model (SM) describes interactions of all known particles with remarkable accuracy Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 2 Fundamental Problems > Standard Model (SM) describes interactions of all known particles with remarkable accuracy > Big fundamental problems in par- ticle physics and cosmology seem to require new physics § Dark matter § Neutrino masses and mixing § Baryon asymmetry § Inflation § Strong CP problem [PLANCK] Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 3 Fundamental Problems > Standard Model (SM) describes interactions of all known particles with remarkable accuracy > Big fundamental problems in par- ticle physics and cosmology seem to require new physics § Dark matter § Neutrino masses and mixing § Baryon asymmetry § Inflation § Strong CP problem > These problems may be intertwin- ed in a minimal way, with a solu- tion pointing to a new physics sca- le around [Ballesteros,Redondo,AR,Tamarit, 1608.05414; 1610.01639] Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 4 Strong CP Problem > Most general gauge invariant Lagrangian of QCD: § Parameters: strong coupling ↵s, quark masses and theta angle [Belavin et al. `75;´t Hooft 76;Callan et al. `76;Jackiw,Rebbi `76 ] Andreas Ringwald | Unifying Inflation with Axion, Dark Matter, Baryogenesis, and Seesaw, Seminar, MPIK HD, D, 13 November 2017 | Page 5 Strong CP Problem > Most general gauge invariant Lagrangian of QCD: § Parameters: strong coupling ↵s, quark masses and theta angle [Belavin et al.
    [Show full text]
  • Exotic Particles in Topological Insulators
    EXOTIC PARTICLES IN TOPOLOGICAL INSULATORS A DISSERTATION SUBMITTED TO THE DEPARTMENT OF PHYSICS AND THE COMMITTEE ON GRADUATE STUDIES OF STANFORD UNIVERSITY IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY Rundong Li July 2010 © 2010 by Rundong Li. All Rights Reserved. Re-distributed by Stanford University under license with the author. This work is licensed under a Creative Commons Attribution- Noncommercial 3.0 United States License. http://creativecommons.org/licenses/by-nc/3.0/us/ This dissertation is online at: http://purl.stanford.edu/yx514yb1109 ii I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. Shoucheng Zhang, Primary Adviser I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. Ian Fisher I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. Steven Kivelson Approved for the Stanford University Committee on Graduate Studies. Patricia J. Gumport, Vice Provost Graduate Education This signature page was generated electronically upon submission of this dissertation in electronic format. An original signed hard copy of the signature page is on file in University Archives. iii Abstract Recently a new class of quantum state of matter, the time-reversal invariant topo- logical insulators, have been theoretically proposed and experimentally discovered.
    [Show full text]
  • L Gauge and Higgs Bosons at the DUNE Near Detector
    FERMILAB-PUB-21-200-T, MI-TH-218 Light, Long-Lived B L Gauge and Higgs Bosons at the DUNE − Near Detector P. S. Bhupal Dev,a Bhaskar Dutta,b Kevin J. Kelly,c Rabindra N. Mohapatra,d Yongchao Zhange;a aDepartment of Physics and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA bMitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, College Station, TX 77845, USA cTheoretical Physics Department, Fermi National Accelerator Laboratory, P. O. Box 500, Batavia, IL 60510, USA dMaryland Center for Fundamental Physics, Department of Physics, University of Maryland, College Park, MD 20742, USA eSchool of Physics, Southeast University, Nanjing 211189, China E-mail: [email protected], [email protected], [email protected], [email protected], [email protected] Abstract: The low-energy U(1)B−L gauge symmetry is well-motivated as part of beyond Standard Model physics related to neutrino mass generation. We show that a light B L gauge boson Z0 and the associated − U(1)B−L-breaking scalar ' can both be effectively searched for at high-intensity facilities such as the near detector complex of the Deep Underground Neutrino Experiment (DUNE). Without the scalar ', the Z0 −9 can be probed at DUNE up to mass of 1 GeV, with the corresponding gauge coupling gBL as low as 10 . In the presence of the scalar ' with gauge coupling to Z0, the DUNE capability of discovering the gauge 0 boson Z can be significantly improved, even by one order of magnitude in gBL, due to additional production from the decay ' Z0Z0.
    [Show full text]
  • Axions (A0) and Other Very Light Bosons, Searches for See the Related Review(S): Axions and Other Similar Particles
    Citation: M. Tanabashi et al. (Particle Data Group), Phys. Rev. D 98, 030001 (2018) Axions (A0) and Other Very Light Bosons, Searches for See the related review(s): Axions and Other Similar Particles A0 (Axion) MASS LIMITS from Astrophysics and Cosmology These bounds depend on model-dependent assumptions (i.e. — on a combination of axion parameters). VALUE (MeV) DOCUMENT ID TECN COMMENT We do not use the following data for averages, fits, limits, etc. ••• ••• >0.2 BARROSO 82 ASTR Standard Axion >0.25 1 RAFFELT 82 ASTR Standard Axion >0.2 2 DICUS 78C ASTR Standard Axion MIKAELIAN 78 ASTR Stellar emission >0.3 2 SATO 78 ASTR Standard Axion >0.2 VYSOTSKII 78 ASTR Standard Axion 1 Lower bound from 5.5 MeV γ-ray line from the sun. 2 Lower bound from requiring the red giants’ stellar evolution not be disrupted by axion emission. A0 (Axion) and Other Light Boson (X 0) Searches in Hadron Decays Limits are for branching ratios. VALUE CL% DOCUMENT ID TECN COMMENT We do not use the following data for averages, fits, limits, etc. ••• ••• <2 10 10 95 1 AAIJ 17AQ LHCB B+ K+ X 0 (X 0 µ+ µ ) × − → → − <3.7 10 8 90 2 AHN 17 KOTO K0 π0 X 0, m = 135 MeV × − L → X 0 11 3 0 0 + <6 10− 90 BATLEY 17 NA48 K± π± X (X µ µ−) × 4 → 0 0 →+ WON 16 BELL η γ X (X π π−) 9 5 0→ 0 0 → 0 + <1 10− 95 AAIJ 15AZ LHCB B K∗ X (X µ µ−) × 6 6 0 → 0 0 →+ <1.5 10− 90 ADLARSON 13 WASA π γ X (X e e−), × m→ = 100 MeV→ X 0 <2 10 8 90 7 BABUSCI 13B KLOE φ η X0 (X 0 e+ e ) × − → → − 8 ARCHILLI 12 KLOE φ η X0, X 0 e+ e → → − <2 10 15 90 9 GNINENKO 12A BDMP π0 γ X 0 (X 0 e+ e ) × − → → −
    [Show full text]
  • On Large Lepton Number Asymmetries of the Universe
    FTUV-17-03-17 IFIC/17-19 On large lepton number asymmetries of the Universe Gabriela Barenboim1∗ and Wan-Il Park2y 1 Departament de F´ısica Te`orica and IFIC, Universitat de Val`encia-CSIC,E-46100, Burjassot, Spain and 2 Department of Science Education (Physics), Chonbuk National University, Jeonju 561-756, Korea (Dated: July 15, 2018) A large lepton number asymmetry of O(0:1 − 1) at present universe might not only be allowed but also necessary for consistency among cosmological data. We show that, if a sizeable lepton number asymmetry were produced before the electroweak phase transition, the requirement for not producing too much baryon number asymmetry through sphalerons processes, forces the high scale lepton number asymmetry to be larger than about 30. Therefore a mild entropy release causing O(10 − 100) suppression of pre-existing particle density should take place, when the background temperature of the universe is around T = O(10−2 − 102)GeV for a large but experimentally consistent asymmetry to be present today. We also show that such a mild entropy production can be obtained by the late-time decays of the saxion, constraining the parameters of the Peccei-Quinn sector such as the mass and the vacuum expectation value of the saxion field to be mφ & O(10)TeV 14 and φ0 & O(10 )GeV, respectively. INTRODUCTION baryon number asymmetry. However, breaking the elec- troweak symmetry requires jLj to be larger than about Extensive analysis of Big Bang Nucleosynthesis (BBN) 10 [10] which is already too large to be consistent with and cosmic microwave background (CMB) data showed CMB data [2].
    [Show full text]
  • Hadronic Axion Model in Gauge-Mediated Supersymmetry
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server TU-558, RCNS-98-20 Hadronic Axion Model in Gauge-Mediated Supersymmetry Breaking and Cosmology of Saxion T. Asaka Institute for Cosmic Ray Research, University of Tokyo, Tanashi 188-8502, Japan Masahiro Yamaguchi Department of Physics, Tohoku University, Sendai 980-8579, Japan (November 1998) Abstract Recently we have proposed a simple hadronic axion model within gauge- mediated supersymmetry breaking. In this paper we discuss various cosmo- logical consequences of the model in great detail. A particular attention is paid to a saxion, a scalar partner of an axion, which is produced as a coherent oscillation in the early universe. We show that our model is cosmologically viable, if the reheating temperature of inflation is sufficiently low. We also discuss the late decay of the saxion which gives a preferable power spectrum of the density fluctuation in the standard cold dark matter model when com- pared with the observation. 1 I. INTRODUCTION The most attractive candidate for the solution of the strong CP problem is the Peccei- Quinn (PQ) mechanism [1]. In this mechanism, there exists an axion which is the Nambu- Goldstone (NG) boson associated with the global U(1)PQ PQ symmetry breaking. In the framework of gauge mediated supersymmetry (SUSY) breaking theories [2], we have proposed an interesting possibility [3] to dynamically generate the PQ symmetry break- ing scale in a so-called hadronic axion model [4]. A gauge singlet PQ multiplet X and colored PQ quark multiplets QP and QP are introduced with the superpotential W = λP XQPQP , (1) where λP is a coupling constant.
    [Show full text]
  • Solving the Tension Between High-Scale Inflation and Axion Isocurvature Perturbations
    JID:PLB AID:30188 /SCO Doctopic: Phenomenology [m5Gv1.3; v 1.134; Prn:15/05/2014; 9:41] P.1(1-6) Physics Letters B ••• (••••) •••–••• 1 Contents lists available at ScienceDirect 66 2 67 3 68 4 Physics Letters B 69 5 70 6 71 7 www.elsevier.com/locate/physletb 72 8 73 9 74 10 75 11 76 12 Solving the tension between high-scale inflation and axion 77 13 isocurvature perturbations 78 14 79 15 Tetsutaro Higaki a, Kwang Sik Jeong b, Fuminobu Takahashi c,d 80 16 81 a 17 Theory Center, KEK, 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan 82 b 18 Deutsches Elektronen Synchrotron DESY, Notkestrasse 85, 22607 Hamburg, Germany 83 c 19 Department of Physics, Tohoku University, Sendai 980-8578, Japan 84 d Kavli IPMU, TODIAS, University of Tokyo, Kashiwa 277-8583, Japan 20 85 21 86 22 87 a r t i c l e i n f o a b s t r a c t 23 88 24 14 89 Article history: The BICEP2 experiment determined the Hubble parameter during inflation to be about 10 GeV. Such 25 90 Received 19 March 2014 high inflation scale is in tension with the QCD axion dark matter if the Peccei–Quinn (PQ) symmetry Received in revised form 21 April 2014 26 remains broken during and after inflation, because too large axion isocurvature perturbations would be 91 Accepted 8 May 2014 27 generated. The axion isocurvature perturbations can be suppressed if the axion acquires a sufficiently 92 Available online xxxx 28 heavy mass during inflation.
    [Show full text]
  • Arxiv:1708.00021V3 [Hep-Ph] 11 Dec 2017
    CTPU-17-30 KIAS-P17058 Minimal Flavor Violation with Axion-like Particles Kiwoon Choia∗, Sang Hui Imby, Chan Beom Parkcz, Seokhoon Yund;ax aCenter for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon 34051, Korea bBethe Center for Theoretical Physics and Physikalisches Institut der Universit¨atBonn Nussallee 12, 53115 Bonn, Germany c School of Physics, Korea Institute for Advanced Study, Seoul 02455, Korea dDepartment of Physics, KAIST, Daejeon 34141, Korea Abstract We revisit the flavor-changing processes involving an axion-like particle (ALP) in the context of generic ALP effective lagrangian with a discussion of possible UV completions providing the origin of the relevant bare ALP couplings. We focus on the minimal scenario that ALP has flavor-conserving couplings at tree level, and the leading flavor-changing couplings arise from the loops involving the Yukawa couplings of the Standard Model fermions. We note that such radiatively generated flavor-changing ALP couplings can be easily suppressed in field theoretic ALP models with sensible UV completion. We discuss also the implication of our result for string theoretic ALP originating from higher-dimensional p-form gauge fields, for instance for ALP in large volume string compactification scenario. arXiv:1708.00021v3 [hep-ph] 11 Dec 2017 ∗ email: [email protected] y email: [email protected] z email: [email protected] x email: [email protected] 1 I. INTRODUCTION Axion-like particle (ALP) is a compelling candidate for physics beyond the standard model (BSM) in the intensity frontier searching for a light particle with feeble interactions to the standard model (SM) particles.
    [Show full text]
  • Strange Terms Used in Used in Theore Cal Physics (Experimenters' View)
    Strange terms used in used in theorecal physics (experimenters’ view) Naturalness - An aesthe*c criterion (not a physical one) leading to expectaon that all free parameters of physical constants appearing in a physical theory should have relave values “of order 1”. This is not a property of the Standard Model where unexplained parameters e.g., masses of fundamental par*cles vary from each other by many orders of magnitude m(electron) = 0.51 MeV vs m(top quark) = 173.2 GeV translated to the size of the corresponding couplings to Higgs boson In the basic formulaon we have two basic constants of nature for weak interac*ons 3 -5 Fermi constant GF/(hc) = 1.166 10 Gev-2 for gravitaon -11 3 -1 -2 -39 2 -2 gravitaonal constant GN = 6.67x10 m kg s = 6.7x10 hc (GeV/c ) Strange terms used in used in theorecal physics Fine-tuning – occurs when the parameters of a model must be adjusted precisely in order to agree with observaons. Models/theories that require fine-tuning adjustments may indicate that there are missing pieces in the theory. This is par*cularly important for cosmological models that have no explanaon for the size of various constants (e.g. cosmological constant, inflaon, etc.) Hierarchy problem – large discrepancy between e.g., weak force and gravity. Weak force is 1032 *mes stronger than gravity. In general, this problem occurs when fundamental value of a parameter used in Lagrangian is different from its effec*ve value measured in experiment. The measured, fundamental value is changed by renormalizaon that includes quantum correc*ons.
    [Show full text]