DOCSLIB.ORG

Kobe University Repository : Kernel

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read 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. a mass around 10−23 eV. The vector field oscillating coher- Recently, however, a consistent ultralight vector model has ently on galactic scales induces oscillations of the spacetime been proposed [11] where the ultralight vector field is homo- metric with a frequency around nHz, which is detectable by geneously condensed during inflation when its mass is less pulsar timing arrays. We find that the pulsar timing signal due than the Hubble scale, and starts to oscillate coherently at to the vector dark matter has nontrivial angular dependence some epoch after inflation. The coherently oscillating vec- unlike the scalar dark matter and the maximal amplitude is tor field behaves as a non-relativistic matter and can be a three times larger than that of the scalar dark matter. candidate for the DM as well as the scalar field. Historically, there have been many works on the vector DM. Evolution of cosmological perturbations based on the 1 Introduction model of ultralight coherent vector DM field has been stud- iedin[12]. There, it is demonstrated that perturbations on Observations of the galactic rotation curves [1], structure the scales smaller than the de Broglie wave length of the formation [2], and gravitational lensing [3] suggest that the vector field have a specific feature compared to the scalar invisible matter, the so-called dark matter (DM) exists in the case. However, the magnitude of the feature is far below the Universe. Searching for the DM has been a long-standing sensitivity of present and future detectors. The approaches to challenge in cosmology and astrophysics. Recent observa- search for the vector DM or to constrain its couplings to parti- tional results show that the DM is accounting for 27% of cles in the Standard Model have been proposed, e.g. by using the energy density in the Universe [4]. The most promising ground-based gravitational-wave interferometers [13,14]or candidate for the DM has been the weak interacting massive taking into account the cosmological plasma effects with a particles (WIMPs) which are motivated by supersymmetric photon [15]. Some phenomenologies on the vector DM are theories of particle physics. However, inspite of the efforts of discussed together with its production mechanism [11,16– many researchers, no signal of the WIMPs has been detected. 23]. The effects of gravitational interaction between the vec- Recently, as an alternative candidate for the DM, an ultra- tor DM field and binary pulsar systems on the dynamics of light axion-like scalar with a mass ∼ 10−23 eV, often called the system have been considered in [24]. the fuzzy DM, has been intensively studied [5,6]. The fuzzy In this paper, we investigate the purely gravitational effects DM has a possibility to resolve small-scale problems of the of the vector DM on the pulsar timing. A coherently oscil- standard Cold DM model such as the galactic core-cusp prob- lating vector field behaves as a non-relativistic pressureless lem [7–9]. matter on cosmological scales. Hence it does not induce the Given the success of the ultralight scalar DM, it is natu- anisotropic expansion of the Universe [25]. Actually, how- ral to ask if the ultralight vector can be the DM. In fact, the ever, there exists an oscillating anisotropic pressure on time possibility of the fuzzy DM being a massive vector boson scales corresponding to the oscillation of the vector field, (sometimes called a dark photon) has been proposed [10,11]. which induces nontrivial oscillations of the metric. The fre- In the case of a vector boson, it is known that it is difficult quency is determined by the mass of the DM considered. In the case of m ∼ 10−23 eV, it is on the order of nHz, which a e-mail: [email protected] (corresponding author) is in the range where the Pulsar Timing Arrays (PTAs) are b e-mail: [email protected] sensitive. PTAs can detect gravitational effects such as grav- c e-mail: [email protected] itational waves [26–28]. Furthermore, a method for detect- 0123456789().: V,-vol 123 419 Page 2 of 10 Eur. Phys. J. C (2020) 80:419 ing the axion-like scalar DM using PTAs has been proposed − 4 − 3 ρ ρ 10 23 eV 10 3 in [29], and actually the energy density of the DM is con- 1095 , m · (mv)3 0.4 GeV/cm3 m v strained by using observational data [30–32]. The detection method is applicable to the case of the vector DM and it is (3) expected that a specific signal depending on the vector prop- ρ erty appears. This is what we will discuss in this paper. where the energy density of the DM is normalized by the This paper is organized as follows. In Sect. 2, we show the local value [33–35]. Since the occupation number is so huge, oscillation of the vector DM field induces time-dependent we can treat the vector field as a classical wave. The de spacetime metric perturbations. In Sect. 3, we see the effect Broglie wavelength for the ultralight vector DM particles of the vector DM on the pulsar timing. We also discuss the withamassm reads detectability of the vector DM with PTAs. In Sect. 4,we 2π 10−23 eV 10−3 summarize the results. Appendix A is devoted to derivation λ = . dB v 4 kpc v (4) of the formula for the redshift of photons induced by metric m m perturbations. Due to the wave nature of the DM field, all inhomogeneities in the DM distribution on the scale smaller than λdB are smoothed out. So we can express the vector DM field as 2 Effects on metric perturbations a superposition of plane waves with a typical wave num- ber k = mv = 2π/λdB. In the present case, the energy In this section, we show that the spacetime metric fluctuates reads E m + mv2/2 m, because the velocity is non- due to the presence of the vector DM oscillating coherently relativistic. Thus, the vector DM field is coherently oscillat- on galactic scales. ing with a monotonic frequency determined by the mass m Since we work on the galactic scales, the cosmic expansion on the scale given by λdB. is negligible. Hence, we consider the metric On galactic scales, we can neglect the cosmic expansion. The equations of motion of the vector field in a flat back- μ ν ds2 = ημνdx dx ground read 2 i j i j − 2(t, x)dt + 2(t, x)δijdx dx + hij(t, x)dx dx , μν 2 ν (1) ∂μ F − m A = 0, (5) where ημν is the Minkowski metric ημν = diag(− 1, + 1, which is derived by taking the variation of the action (2) μν + 1, + 1). The metric perturbations induced by the DM are with respect to Aμ. Using the identity ∂ν∂μ F = 0, we can described by , , and hij. Weshall discuss the perturbations rewrite Eq. ((5)) as a set of Proca equations in the standard separately in Eqs. (18) and (25). form: The vector DM field Aμ with a mass m is expected to μ have little interaction with particles in the Standard Model. ∂μ A = 0, (6) We treat the vector DM field as a free field. Its action is given (−∂2 + ∇2 − 2) μ = . 0 m A 0 (7) by √ Taking into account that the field typically has a frequency 4 1 μν ρσ 1 2 μν S = d x −g − g g Fμρ Fνσ − m g Aμ Aν , m and a momentum k,Eq.((6)) gives 4 2 (2) k A ∼ A . (8) t m i where g is the determinant of the metric gμν and Fμν = ∂ − ∂ −3 μ Aν ν Aμ. We also consider the ultralight mass of the Hence, At gets suppressed by the order of k/m = v ∼ 10 ∼ −23 vector DM as m 10 eV, which can arise through the compared to Ai .
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]
  • 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]
  • 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]
  • 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]
  • A Study of Fermionic Dark Matter with a Z-Prime Portal
    How was Dark Matter produced in the early universe? A study of fermionic Dark Matter with a Z-prime portal by Taylor Rose Gray A thesis submitted to the Faculty of Graduate and Postdoctoral Affairs in partial fulfillment of the requirements for the degree of Master of Science in Particle Physics Department of Physics Carleton University Ottawa-Carleton Institute of Physics Ottawa, Canada Copyright c 2020 Taylor Rose Gray Abstract We study a model of fermionic dark matter interacting with the Standard Model through a sequential Z0 mediator, the gauge boson of a U(1) extension to the Standard Model symmetry group, to understand the mechanism responsible for the dark matter relic abundance. We compare two different mechanisms for dark matter production in the early universe, freeze-out and freeze-in. For production through freeze-out, dark matter particles were in thermal equilibrium with the cosmic plasma until the expansion of the universe dominated over the interactions. For freeze-in, dark matter was never in thermal equilibrium with the visible sector, and its abundance is always negligible compared to the thermal bath abundances. The boundary between each production regime is explored by considering every free parameter of this model, namely the masses and couplings. Details of the boundary region between freeze-in and freeze-out could have implications for dark matter searches. ii Acknowledgments Throughout the entire process that writing this thesis entailed, I have received an immense amount of support, guidance, and patience. First, I wish to show my deepest gratitude to my supervisor, Stephen Godfrey, who has taught me more than I could have imagined learning in my degree.
    [Show full text]
  • Techniques for Inelastic Effective Field Theory Measurements with The
    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]
  • Springer Proceedings in Physics
    Springer Proceedings in Physics Volume 148 For further volumes: http://www.springer.com/series/361 David Cline Editor Sources and Detection of Dark Matter and Dark Energy in the Universe Proceedings of the 10th UCLA Symposium on Sources and Detection of Dark Matter and Dark Energy in the Universe, February 22-24, 2012, Marina del Rey, California Editor David Cline UCLA Physics & Astronomy Los Angeles , USA ISSN 0930-8989 ISSN 1867-4941 (electronic) ISBN 978-94-007-7240-3 ISBN 978-94-007-7241-0 (eBook) DOI 10.1007/978-94-007-7241-0 Springer Dordrecht Heidelberg New York London Library of Congress Control Number: 2013955385 © Springer Science+Business Media Dordrecht 2013 This work is subject to copyright. All rights are reserved by the Publisher, whether the whole or part of the material is concerned, specifi cally the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfi lms or in any other physical way, and transmission or information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed. Exempted from this legal reservation are brief excerpts in connection with reviews or scholarly analysis or material supplied specifi cally for the purpose of being entered and executed on a computer system, for exclusive use by the purchaser of the work. Duplication of this publication or parts thereof is permitted only under the provisions of the Copyright Law of the Publisher’s location, in its current version, and permission for use must always be obtained from Springer. Permissions for use may be obtained through RightsLink at the Copyright Clearance Center.
    [Show full text]
  • Can Dark Matter Be a Scalar Field? Portal John March-Russell, Stephen M
    Journal of Cosmology and Astroparticle Physics Related content - Heavy dark matter through the Higgs Can dark matter be a scalar field? portal John March-Russell, Stephen M. West, Daniel Cumberbatch et al. To cite this article: J.F. Jesus et al JCAP08(2016)046 - Simulated Milky Way analogues: implications for dark matter direct searches Nassim Bozorgnia, Francesca Calore, Matthieu Schaller et al. View the article online for updates and enhancements. - Dark matter in song Recent citations - Oscillatons described by self–interacting quartic scalar fields A. Mahmoodzadeh and B. Malakolkalami This content was downloaded from IP address 186.217.236.64 on 17/06/2019 at 19:16 ournal of Cosmology and Astroparticle Physics JAn IOP and SISSA journal Can dark matter be a scalar field? JCAP08(2016)046 J.F. Jesus,a S.H. Pereira,b J.L.G. Malatrasia and F. Andrade-Oliveirac aUniversidade Estadual Paulista “J´ulio de Mesquita Filho”, Campus Experimental de Itapeva — R. Geraldo Alckmin, 519, Itapeva, SP, Brazil bUniversidade Estadual Paulista “J´ulio de Mesquita Filho”, Departamento de F´ısica e Qu´ımica, Campus de Guaratinguet´a, Av. Dr. Ariberto Pereira da Cunha, 333, 12516-410 — Guaratinguet´a, SP, Brazil cInstitute of Cosmology and Gravitation, University of Portsmouth, Burnaby Road, PO1 3FX, Portsmouth, U.K. E-mail: [email protected], [email protected], [email protected], [email protected] Received April 28, 2016 Revised July 22, 2016 Accepted August 9, 2016 Published August 22, 2016 Abstract. In this paper we study a real scalar field as a possible candidate to explain the dark matter in the universe.
    [Show full text]
  • Ultra-Light Dark Matter
    Noname manuscript No. (will be inserted by the editor) Ultra-light dark matter Elisa G. M. Ferreira the date of receipt and acceptance should be inserted later Abstract Ultra-light dark matter is a class of dark matter models (DM) where DM is composed by bosons with masses ranging from 10−24 eV < m < eV. These models have been receiving a lot of attention in the past few years given their interesting property of forming a Bose{Einstein condensate (BEC) or a superfluid on galactic scales. BEC and superfluidity are some of the most striking quantum mechanical phenomena manifest on macroscopic scales, and upon condensation the particles behave as a single coherent state, described by the wavefunction of the condensate. The idea is that condensation takes place inside galaxies while outside, on large scales, it recovers the successes of ΛCDM. This wave nature of DM on galactic scales that arise upon condensation can address some of the curiosities of the behaviour of DM on small scales. There are many models in the literature that describe a DM component that condenses in galaxies. In this review, we are going to describe those models, and classify them into three classes, according to the different non-linear evolution and structures they form in galaxies: the fuzzy dark matter (FDM), the self-interacting fuzzy dark matter (SIFDM), and the DM superfluid. Each of these classes comprises many models, each presenting a similar phenomenology in galaxies. They also include some microscopic models like the axions and axion-like particles. To understand and describe this phenomenology in galaxies, we are going to review the phenomena of BEC and superfluidity that arise in condensed matter physics, and apply this knowledge to DM.
    [Show full text]