Fuzzy and Axion-Like Dark Matter As an Illusion
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Fuzzy Cold Dark Matter: the Wave Properties of Ultralight Particles
VOLUME 85, NUMBER 6 PHYSICAL REVIEW LETTERS 7AUGUST 2000 Fuzzy Cold Dark Matter: The Wave Properties of Ultralight Particles Wayne Hu, Rennan Barkana, and Andrei Gruzinov Institute for Advanced Study, Princeton, New Jersey 08540 (Received 27 March 2000) Cold dark matter (CDM) models predict small-scale structure in excess of observations of the cores and abundance of dwarf galaxies. These problems might be solved, and the virtues of CDM models retained, even without postulating ad hoc dark matter particle or field interactions, if the dark matter is composed of ultralight scalar particles ͑m ϳ 10222 eV͒, initially in a (cold) Bose-Einstein condensate, similar to axion dark matter models. The wave properties of the dark matter stabilize gravitational collapse, providing halo cores and sharply suppressing small-scale linear power. PACS numbers: 95.35.+d, 98.80.Cq Introduction.—Recently, the small-scale shortcomings particle horizon, one can employ a Newtonian approxi- of the otherwise widely successful cold dark matter (CDM) mation to the gravitational interaction embedded in the models for structure formation have received much atten- covariant derivatives of the field equation and a nonrela- tion (see [1–4] and references therein). CDM models pre- tivistic approximation to the dispersion relation. It is then dict cuspy dark matter halo profiles and an abundance of convenient to define the wave function c ϵ Aeia, out of low mass halos not seen in the rotation curves and local the amplitude and phase of the field f A cos͑mt 2a͒, population of dwarf galaxies, respectively. Although the which obeys µ ∂ µ ∂ significance of the discrepancies is still disputed and so- ᠨ 3 a 1 2 lutions involving astrophysical processes in the baryonic i ≠t 1 c 2 = 1 mC c , (2) gas may still be possible (e.g., [5]), recent attention has fo- 2 a 2m cused mostly on solutions involving the dark matter sector. -
Galaxy Formation with Ultralight Bosonic Dark Matter
GALAXY FORMATION WITH ULTRALIGHT BOSONIC DARK MATTER Dissertation zur Erlangung des mathematisch-naturwissenschaftlichen Doktorgrades "Doctor rerum naturalium" der Georg-August-Universit¨atG¨ottingen im Promotionsstudiengang Physik der Georg-August University School of Science (GAUSS) vorgelegt von Jan Veltmaat aus Bietigheim-Bissingen G¨ottingen,2019 Betreuungsausschuss Prof. Dr. Jens Niemeyer, Institut f¨urAstrophysik, Universit¨atG¨ottingen Prof. Dr. Steffen Schumann, Institut f¨urTheoretische Physik, Universit¨atG¨ottingen Mitglieder der Pr¨ufungskommission Referent: Prof. Dr. Jens Niemeyer, Institut f¨urAstrophysik, Universit¨atG¨ottingen Korreferent: Prof. Dr. David Marsh, Institut f¨urAstrophysik, Universit¨atG¨ottingen Weitere Mitglieder der Pr¨ufungskommission: Prof. Dr. Fabian Heidrich-Meisner, Institut f¨urTheoretische Physik, Universit¨atG¨ottingen Prof. Dr. Wolfram Kollatschny, Institut f¨urAstrophysik, Universit¨atG¨ottingen Prof. Dr. Steffen Schumann, Institut f¨urTheoretische Physik, Universit¨atG¨ottingen Dr. Michael Wilczek, Max-Planck-Institut f¨urDynamik und Selbstorganisation, G¨ottingen Tag der m¨undlichen Pr¨ufung:12.12.2019 Abstract Ultralight bosonic particles forming a coherent state are dark matter candidates with distinctive wave-like behaviour on the scale of dwarf galaxies and below. In this thesis, a new simulation technique for ul- tralight bosonic dark matter, also called fuzzy dark matter, is devel- oped and applied in zoom-in simulations of dwarf galaxy halos. When gas and star formation are not included in the simulations, it is found that halos contain solitonic cores in their centers reproducing previous results in the literature. The cores exhibit strong quasi-normal oscil- lations, which are possibly testable by observations. The results are inconclusive regarding the long-term evolution of the core mass. -
Small Scale Problems of the CDM Model
galaxies Article Small Scale Problems of the LCDM Model: A Short Review Antonino Del Popolo 1,2,3,* and Morgan Le Delliou 4,5,6 1 Dipartimento di Fisica e Astronomia, University of Catania , Viale Andrea Doria 6, 95125 Catania, Italy 2 INFN Sezione di Catania, Via S. Sofia 64, I-95123 Catania, Italy 3 International Institute of Physics, Universidade Federal do Rio Grande do Norte, 59012-970 Natal, Brazil 4 Instituto de Física Teorica, Universidade Estadual de São Paulo (IFT-UNESP), Rua Dr. Bento Teobaldo Ferraz 271, Bloco 2 - Barra Funda, 01140-070 São Paulo, SP Brazil; [email protected] 5 Institute of Theoretical Physics Physics Department, Lanzhou University No. 222, South Tianshui Road, Lanzhou 730000, Gansu, China 6 Instituto de Astrofísica e Ciências do Espaço, Universidade de Lisboa, Faculdade de Ciências, Ed. C8, Campo Grande, 1769-016 Lisboa, Portugal † [email protected] Academic Editors: Jose Gaite and Antonaldo Diaferio Received: 30 May 2016; Accepted: 9 December 2016; Published: 16 February 2017 Abstract: The LCDM model, or concordance cosmology, as it is often called, is a paradigm at its maturity. It is clearly able to describe the universe at large scale, even if some issues remain open, such as the cosmological constant problem, the small-scale problems in galaxy formation, or the unexplained anomalies in the CMB. LCDM clearly shows difficulty at small scales, which could be related to our scant understanding, from the nature of dark matter to that of gravity; or to the role of baryon physics, which is not well understood and implemented in simulation codes or in semi-analytic models. -
A Unifying Theory of Dark Energy and Dark Matter: Negative Masses and Matter Creation Within a Modified ΛCDM Framework J
Astronomy & Astrophysics manuscript no. theory_dark_universe_arxiv c ESO 2018 November 5, 2018 A unifying theory of dark energy and dark matter: Negative masses and matter creation within a modified ΛCDM framework J. S. Farnes1; 2 1 Oxford e-Research Centre (OeRC), Department of Engineering Science, University of Oxford, Oxford, OX1 3QG, UK. e-mail: [email protected]? 2 Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, NL-6500 GL Nijmegen, the Netherlands. Received February 23, 2018 ABSTRACT Dark energy and dark matter constitute 95% of the observable Universe. Yet the physical nature of these two phenomena remains a mystery. Einstein suggested a long-forgotten solution: gravitationally repulsive negative masses, which drive cosmic expansion and cannot coalesce into light-emitting structures. However, contemporary cosmological results are derived upon the reasonable assumption that the Universe only contains positive masses. By reconsidering this assumption, I have constructed a toy model which suggests that both dark phenomena can be unified into a single negative mass fluid. The model is a modified ΛCDM cosmology, and indicates that continuously-created negative masses can resemble the cosmological constant and can flatten the rotation curves of galaxies. The model leads to a cyclic universe with a time-variable Hubble parameter, potentially providing compatibility with the current tension that is emerging in cosmological measurements. In the first three-dimensional N-body simulations of negative mass matter in the scientific literature, this exotic material naturally forms haloes around galaxies that extend to several galactic radii. These haloes are not cuspy. The proposed cosmological model is therefore able to predict the observed distribution of dark matter in galaxies from first principles. -
Self-Interacting Inelastic Dark Matter: a Viable Solution to the Small Scale Structure Problems
Prepared for submission to JCAP ADP-16-48/T1004 Self-interacting inelastic dark matter: A viable solution to the small scale structure problems Mattias Blennow,a Stefan Clementz,a Juan Herrero-Garciaa; b aDepartment of physics, School of Engineering Sciences, KTH Royal Institute of Tech- nology, AlbaNova University Center, 106 91 Stockholm, Sweden bARC Center of Excellence for Particle Physics at the Terascale (CoEPP), University of Adelaide, Adelaide, SA 5005, Australia Abstract. Self-interacting dark matter has been proposed as a solution to the small- scale structure problems, such as the observed flat cores in dwarf and low surface brightness galaxies. If scattering takes place through light mediators, the scattering cross section relevant to solve these problems may fall into the non-perturbative regime leading to a non-trivial velocity dependence, which allows compatibility with limits stemming from cluster-size objects. However, these models are strongly constrained by different observations, in particular from the requirements that the decay of the light mediator is sufficiently rapid (before Big Bang Nucleosynthesis) and from direct detection. A natural solution to reconcile both requirements are inelastic endothermic interactions, such that scatterings in direct detection experiments are suppressed or even kinematically forbidden if the mass splitting between the two-states is sufficiently large. Using an exact solution when numerically solving the Schr¨odingerequation, we study such scenarios and find regions in the parameter space of dark matter and mediator masses, and the mass splitting of the states, where the small scale structure problems can be solved, the dark matter has the correct relic abundance and direct detection limits can be evaded. -
Probing the Nature of Dark Matter in the Universe
PROBING THE NATURE OF DARK MATTER IN THE UNIVERSE A Thesis Submitted For The Degree Of Doctor Of Philosophy In The Faculty Of Science by Abir Sarkar Under the supervision of Prof. Shiv K Sethi Raman Research Institute Joint Astronomy Programme (JAP) Department of Physics Indian Institute of Science BANGALORE - 560012 JULY, 2017 c Abir Sarkar JULY 2017 All rights reserved Declaration I, Abir Sarkar, hereby declare that the work presented in this doctoral thesis titled `Probing The Nature of Dark Matter in the Universe', is entirely original. This work has been carried out by me under the supervision of Prof. Shiv K Sethi at the Department of Astronomy and Astrophysics, Raman Research Institute under the Joint Astronomy Programme (JAP) of the Department of Physics, Indian Institute of Science. I further declare that this has not formed the basis for the award of any degree, diploma, membership, associateship or similar title of any university or institution. Department of Physics Abir Sarkar Indian Institute of Science Date : Bangalore, 560012 INDIA TO My family, without whose support this work could not be done Acknowledgements First and foremost I would like to thank my supervisor Prof. Shiv K Sethi in Raman Research Institute(RRI). He has always spent substantial time whenever I have needed for any academic discussions. I am thankful for his inspirations and ideas to make my Ph.D. experience produc- tive and stimulating. I am also grateful to our collaborator Prof. Subinoy Das of Indian Institute of Astrophysics, Bangalore, India. I am thankful to him for his insightful comments not only for our publica- tions but also for the thesis. -
Dynamical Friction in a Fuzzy Dark Matter Universe
Prepared for submission to JCAP Dynamical Friction in a Fuzzy Dark Matter Universe Lachlan Lancaster ,a;1 Cara Giovanetti ,b Philip Mocz ,a;2 Yonatan Kahn ,c;d Mariangela Lisanti ,b David N. Spergel a;b;e aDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ, 08544, USA bDepartment of Physics, Princeton University, Princeton, New Jersey, 08544, USA cKavli Institute for Cosmological Physics, University of Chicago, Chicago, IL, 60637, USA dUniversity of Illinois at Urbana-Champaign, Urbana, IL, 61801, USA eCenter for Computational Astrophysics, Flatiron Institute, NY, NY 10010, USA E-mail: [email protected], [email protected], [email protected], [email protected], [email protected], dspergel@flatironinstitute.org Abstract. We present an in-depth exploration of the phenomenon of dynamical friction in a universe where the dark matter is composed entirely of so-called Fuzzy Dark Matter (FDM), ultralight bosons of mass m ∼ O(10−22) eV. We review the classical treatment of dynamical friction before presenting analytic results in the case of FDM for point masses, extended mass distributions, and FDM backgrounds with finite velocity dispersion. We then test these results against a large suite of fully non-linear simulations that allow us to assess the regime of applicability of the analytic results. We apply these results to a variety of astrophysical problems of interest, including infalling satellites in a galactic dark matter background, and −21 −2 determine that (1) for FDM masses m & 10 eV c , the timing problem of the Fornax dwarf spheroidal’s globular clusters is no longer solved and (2) the effects of FDM on the process of dynamical friction for satellites of total mass M and relative velocity vrel should 9 −22 −1 require detailed numerical simulations for M=10 M m=10 eV 100 km s =vrel ∼ 1, parameters which would lie outside the validated range of applicability of any currently developed analytic theory, due to transient wave structures in the time-dependent regime. -
Department of Physics and Astronomy University of Heidelberg Tim
Department of Physics and Astronomy University of Heidelberg Master Thesis in Physics submitted by Tim Zimmermann born in Nürtingen (Germany) 2020 An Investigation of the Lower Dimensional Dynamics of Fuzzy Dark Matter This Master Thesis has been carried out by Tim Zimmermann at the Institute for Theoretical Physics under the supervision of Prof. Dr. Luca Amendola and Prof. Dr. Sandro Wimberger. Abstract Due to the lack of experimental evidence for weakly interacting particles (WIMPs) and the unsatisfying numerical predictions of the established cold dark matter (CDM) paradigm on galactic scales, alternative dark matter models remain an intriguing and active field of research. A model of recent interest in cosmology is Fuzzy Dark Matter (FDM) which assumes the nonbaryonic matter component of the universe to consist of scalar bosons with mass m 10−22 eV. FDM possesses a rich phenomenology in (3 + 1) dimensions recovering predictions∼ of CDM on large scales while suppressing structure growth below the de-Broglie wavelength which, due to the miniscule boson mass, attains values of galactic size. As full fledged (3 + 1)-dimensional, cosmological simulations, especially for FDM, are extremely time consuming this thesis investigates to what extend phenomena in three spatial dimensions can be observed with only one geometric degree of freedom. To this end, a first principle derivation of the governing equation of FDM, i.e. (3 + 1)- Schrödinger-Poisson (SP) is presented and dimensionally reduced to two distinct (1 + 1)-FDM representations, namely (i) the standard (1 + 1)-SP equation and (ii) the novel periodic, line adiabatic model (PLAM). After investigating the nature of FDM in linear theory, we present a comprehensive, unified and thoroughly tested numerical method capable of integrating both reduction models into the nonlinear regime. -
'Dark Matter Halo for Every Elementary Particle' Model
A critical review of MOND from the perspective of the `Dark Matter Halo for Every Elementary Particle' Model E.P.J. de Haas (Paul) Nijmegen, The Netherlands∗ (Dated: September 24, 2015) Abstract In this paper I look at MOND from the perspective of my elementary particle Dark matter halo hypothesis. First I repeat the core elements of my model, in order for the paper to be self contained. Then I show how the energy equation for the rotation curve with an extra constant term can give the natural but deceptive impression that Newton's Laws have to be corrected for the ultra low regime, if this energy perspective is missing. Special attention is given to the virtual aspect of the acceleration, virtual as in not caused by Newton's force of gravity, due to a constant kinetic energy caused by the Dark Matter halo at large distances. The rotation curve equations are discussed and the one from my model is given. Conclusions are drawn from the ΛCDM core-cusp problem in relation to this new perspective on MOND as hiding a Dark Matter model perspective. My model might well be the bridge between MOND at the galactic scale and ΛCDM at the cosmic level. ∗ haas2u[at]gmail.com 1 I. THE ELEMENTARY PARTICLE DARK MATTER HALO MODEL It is common knowledge that a Dark Matter mass function linear in r can explain the flatness of galaxy rotation curves at large r. This is the empirical starting point of our Dark Matter model, first presented in [1] and in [2]. Given a rest mass m0 at r = 0, it will have an additional spherical Dark Matter halo containing an extra mass, with Dark Matter properties only, in the sphere with radius r as r mdm = m0: (1) rdm The Dark Matter radius rdm should have a galaxy specific value somewhere in between 10 kpc and 20 kpc, so approximately once or twice the radius of an average luminous galaxy. -
![Arxiv:2101.01282V1 [Astro-Ph.GA] 4 Jan 2021 Wang Et Al](https://docslib.b-cdn.net/cover/7943/arxiv-2101-01282v1-astro-ph-ga-4-jan-2021-wang-et-al-3217943.webp)
Arxiv:2101.01282V1 [Astro-Ph.GA] 4 Jan 2021 Wang Et Al
Draft version January 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 A cuspy dark matter halo Yong Shi,1, 2 Zhi-Yu Zhang,1, 2 Junzhi Wang,3 Jianhang Chen,1 Qiusheng Gu,1, 2 Xiaoling Yu,1 and Songlin Li1 1School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China. 2Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China. 3Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China ABSTRACT The cusp-core problem is one of the main challenges of the cold dark matter paradigm on small scales: the density of a dark matter halo is predicted to rise rapidly toward the center as ρ(r) / rα with α between -1 and -1.5, while such a cuspy profile has not been clearly observed. We have carried out the spatially-resolved mapping of gas dynamics toward a nearby ultra-diffuse galaxy (UDG), AGC 242019. The derived rotation curve of dark matter is well fitted by the cuspy profile as described by the Navarro-Frenk-White model, while the cored profiles including both the pseudo-isothermal and Burkert models are excluded. The halo has α= -(0.90±0.08) at the innermost radius of 0.67 kpc , 10 Mhalo=(3.5±1.2)×10 M and a small concentration of 2.0±0.36. AGC 242019 challenges alternatives of cold dark matter by constraining the particle mass of fuzzy dark matter to be < 0.11×10−22 eV or > 3.3×10−22 eV , the cross section of self-interacting dark matter to be < 1.63 cm2/g, and the particle mass of warm dark matter to be > 0.23 keV, all of which are in tension with other constraints. -
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. -
A Unifying Theory of Dark Energy and Dark Matter: Negative Masses and Matter Creation Within a Modified ΛCDM Framework?,?? J
A&A 620, A92 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832898 & c ESO 2018 Astrophysics A unifying theory of dark energy and dark matter: Negative masses and matter creation within a modified ΛCDM framework?,?? J. S. Farnes1,2 1 Oxford e-Research Centre (OeRC), Department of Engineering Science, University of Oxford, Oxford OX1 3QG, UK e-mail: [email protected] 2 Department of Astrophysics/IMAPP, Radboud University, PO Box 9010, 6500 GL Nijmegen, The Netherlands Received 22 February 2018 / Accepted 20 October 2018 ABSTRACT Dark energy and dark matter constitute 95% of the observable Universe. Yet the physical nature of these two phenomena remains a mystery. Einstein suggested a long-forgotten solution: gravitationally repulsive negative masses, which drive cosmic expansion and cannot coalesce into light-emitting structures. However, contemporary cosmological results are derived upon the reasonable assumption that the Universe only contains positive masses. By reconsidering this assumption, I have constructed a toy model which suggests that both dark phenomena can be unified into a single negative mass fluid. The model is a modified ΛCDM cosmology, and indicates that continuously-created negative masses can resemble the cosmological constant and can flatten the rotation curves of galaxies. The model leads to a cyclic universe with a time-variable Hubble parameter, potentially providing compatibility with the current tension that is emerging in cosmological measurements. In the first three-dimensional N-body simulations of negative mass matter in the scientific literature, this exotic material naturally forms haloes around galaxies that extend to several galactic radii. These haloes are not cuspy.