What Is Dark Matter?
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Dark Energy and Dark Matter As Inertial Effects Introduction
Dark Energy and Dark Matter as Inertial Effects Serkan Zorba Department of Physics and Astronomy, Whittier College 13406 Philadelphia Street, Whittier, CA 90608 [email protected] ABSTRACT A disk-shaped universe (encompassing the observable universe) rotating globally with an angular speed equal to the Hubble constant is postulated. It is shown that dark energy and dark matter are cosmic inertial effects resulting from such a cosmic rotation, corresponding to centrifugal (dark energy), and a combination of centrifugal and the Coriolis forces (dark matter), respectively. The physics and the cosmological and galactic parameters obtained from the model closely match those attributed to dark energy and dark matter in the standard Λ-CDM model. 20 Oct 2012 Oct 20 ph] - PACS: 95.36.+x, 95.35.+d, 98.80.-k, 04.20.Cv [physics.gen Introduction The two most outstanding unsolved problems of modern cosmology today are the problems of dark energy and dark matter. Together these two problems imply that about a whopping 96% of the energy content of the universe is simply unaccounted for within the reigning paradigm of modern cosmology. arXiv:1210.3021 The dark energy problem has been around only for about two decades, while the dark matter problem has gone unsolved for about 90 years. Various ideas have been put forward, including some fantastic ones such as the presence of ghostly fields and particles. Some ideas even suggest the breakdown of the standard Newton-Einstein gravity for the relevant scales. Although some progress has been made, particularly in the area of dark matter with the nonstandard gravity theories, the problems still stand unresolved. -
Dark Matter and the Dinosaurs: the Astounding Interconnectedness of the Universe Pdf, Epub, Ebook
DARK MATTER AND THE DINOSAURS: THE ASTOUNDING INTERCONNECTEDNESS OF THE UNIVERSE PDF, EPUB, EBOOK Lisa Randall | 432 pages | 05 Jan 2017 | Vintage Publishing | 9780099593560 | English | London, United Kingdom Dark Matter and the Dinosaurs: The Astounding Interconnectedness of the Universe PDF Book Randall rebuts such criticism by noting that it could be "simpler to say that dark matter is like our matter, in that it's different particles with different forces", adding "the other answer is that the world's complicated, so Occam's razor isn't always the best way to go about things. There was a problem filtering reviews right now. Creo que su lectura es muy recomendable. So if, in fact, there is this dense, dark disk, there should be evidence for it in this data, which will be really exciting. Amazon Second Chance Pass it on, trade it in, give it a second life. Retrieved 12 December Or, if you are already a subscriber Sign in. Randall: I mean there is, of course, also the richness of how the pieces fit together, which is the wonderful stuff that we observe in the world. And second, once we have them, what are all the consequences? Randall conjectures that dark matter may have indirectly led to the extinction of dinosaurs. And those are worth drilling down and really focusing on. Introduction is nice and smooth. And we can see how that fits together and then how that came about and try to understand that with science, over time. Baird, Jr. Although I am left confused to wether there is evidence for periodicity or not. -
Dark Matter and the Early Universe: a Review Arxiv:2104.11488V1 [Hep-Ph
Dark matter and the early Universe: a review A. Arbey and F. Mahmoudi Univ Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, Institut de Physique des 2 Infinis de Lyon, UMR 5822, 69622 Villeurbanne, France Theoretical Physics Department, CERN, CH-1211 Geneva 23, Switzerland Institut Universitaire de France, 103 boulevard Saint-Michel, 75005 Paris, France Abstract Dark matter represents currently an outstanding problem in both cosmology and particle physics. In this review we discuss the possible explanations for dark matter and the experimental observables which can eventually lead to the discovery of dark matter and its nature, and demonstrate the close interplay between the cosmological properties of the early Universe and the observables used to constrain dark matter models in the context of new physics beyond the Standard Model. arXiv:2104.11488v1 [hep-ph] 23 Apr 2021 1 Contents 1 Introduction 3 2 Standard Cosmological Model 3 2.1 Friedmann-Lema^ıtre-Robertson-Walker model . 4 2.2 A quick story of the Universe . 5 2.3 Big-Bang nucleosynthesis . 8 3 Dark matter(s) 9 3.1 Observational evidences . 9 3.1.1 Galaxies . 9 3.1.2 Galaxy clusters . 10 3.1.3 Large and cosmological scales . 12 3.2 Generic types of dark matter . 14 4 Beyond the standard cosmological model 16 4.1 Dark energy . 17 4.2 Inflation and reheating . 19 4.3 Other models . 20 4.4 Phase transitions . 21 5 Dark matter in particle physics 21 5.1 Dark matter and new physics . 22 5.1.1 Thermal relics . 22 5.1.2 Non-thermal relics . -
Effective Description of Dark Matter As a Viscous Fluid
Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Effective Description of Dark Matter as a Viscous Fluid Nikolaos Tetradis University of Athens Work with: D. Blas, S. Floerchinger, M. Garny, U. Wiedemann . N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Distribution of dark and baryonic matter in the Universe Figure: 2MASS Galaxy Catalog (more than 1.5 million galaxies). N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Inhomogeneities Inhomogeneities are treated as perturbations on top of an expanding homogeneous background. Under gravitational attraction, the matter overdensities grow and produce the observed large-scale structure. The distribution of matter at various redshifts reflects the detailed structure of the cosmological model. Define the density field δ = δρ/ρ0 and its spectrum hδ(k)δ(q)i ≡ δD(k + q)P(k): . N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid 31 timation method in its entirety, but it should be equally valid. 7.3. Comparison to other results Figure 35 compares our results from Table 3 (modeling approach) with other measurements from galaxy surveys, but must be interpreted with care. The UZC points may contain excess large-scale power due to selection function effects (Padmanabhan et al. 2000; THX02), and the an- gular SDSS points measured from the early data release sample are difficult to interpret because of their extremely broad window functions. -
Understanding a Warped Cosmos
Lisa Randall. “One challenge today is to see what you can do with large amounts of data, to study fundamental properties, not just questions of how electromagnetism gives rise to certain things. Can we actually see deviations from what you would predict in conventional theories?” Rami Shllush Understanding a warped cosmos What’s the connection between dinosaurs and dark matter? What is the glue that holds the universe together? Is there a fourth - and fifth - dimension? These are just some of the questions that occupy Lisa Randall, the first female physicist to get tenure at Princeton, Harvard and MIT ■ ״ ״r* י •• 1 י׳ The CERN facility, near Geneva. “We need higher-energy machines and particle Illustration of a large asteroid colliding with Earth over the Yucatan Peninsula, in accelerators,” says Randall, “but to really see new things, we need even more Mexico. The impact of such occurrences are thought to have led to the death of the powerful machines.” Richard Juillian/AFP dinosaurs some 65 million years ago. Mark Garlick/Science Photo Libra Ido Efrati in the sciences. In 2016 he mystery of the universe,be seen as evidence that dark matter Over the years, studies have specializes interview with The New she and the many riddles that re- interacted in some way with hydrogen mapped the presence of dark matter Yorker, related that in her teens she had fre- main open about itcan be ex- atoms, thus leadingto the loweringof in various placesin the universe,in- the of the dark matter. our emplifiedin myriad ways. temperature eludingin the center of galaxy,the quent confrontations with her mother, to One of the most frustratingPhysicistsresponding the article Milky Way. -
Modified Newtonian Dynamics
J. Astrophys. Astr. (December 2017) 38:59 © Indian Academy of Sciences https://doi.org/10.1007/s12036-017-9479-0 Modified Newtonian Dynamics (MOND) as a Modification of Newtonian Inertia MOHAMMED ALZAIN Department of Physics, Omdurman Islamic University, Omdurman, Sudan. E-mail: [email protected] MS received 2 February 2017; accepted 14 July 2017; published online 31 October 2017 Abstract. We present a modified inertia formulation of Modified Newtonian dynamics (MOND) without retaining Galilean invariance. Assuming that the existence of a universal upper bound, predicted by MOND, to the acceleration produced by a dark halo is equivalent to a violation of the hypothesis of locality (which states that an accelerated observer is pointwise inertial), we demonstrate that Milgrom’s law is invariant under a new space–time coordinate transformation. In light of the new coordinate symmetry, we address the deficiency of MOND in resolving the mass discrepancy problem in clusters of galaxies. Keywords. Dark matter—modified dynamics—Lorentz invariance 1. Introduction the upper bound is inferred by writing the excess (halo) acceleration as a function of the MOND acceleration, The modified Newtonian dynamics (MOND) paradigm g (g) = g − g = g − gμ(g/a ). (2) posits that the observations attributed to the presence D N 0 of dark matter can be explained and empirically uni- It seems from the behavior of the interpolating function fied as a modification of Newtonian dynamics when the as dictated by Milgrom’s formula (Brada & Milgrom gravitational acceleration falls below a constant value 1999) that the acceleration equation (2) is universally −10 −2 of a0 10 ms . -
Minutes High Energy Physics Advisory Panel October 22–23, 2009 Hilton Embassy Row Washington, D.C
Draft Minutes High Energy Physics Advisory Panel October 22–23, 2009 Hilton Embassy Row Washington, D.C. HEPAP members present: Hiroaki Aihara Wim Leemans Marina Artuso Daniel Marlow Alice Bean Ann Nelson Patricia Burchat Paris Sphicas Lance Dixon Kate Scholberg Graciela Gelmini Melvyn J. Shochet, Chair Larry Gladney Henry Sobel Boris Kayser Maury Tigner Robert Kephart William Trischuk Steven Kettell Herman White HEPAP members absent: Priscilla Cushman Lisa Randall Sarah Eno Sally Seidel Stephen Olson Also participating: Barry Barish, Director, Global Design Effort, International Linear Collider Frederick Bernthal, President, Universities Research Association Glen Crawford, HEPAP Designated Federal Officer, Office of High Energy Physics, Office of Science, Department of Energy Joseph Dehmer, Director, Division of Physics, National Science Foundation Cristinel Diaconu, Directeur de Recherche, IN2P3/CNRS, France Robert Diebold, Diebold Consulting Marvin Goldberg, Program Director, Division of Physics, National Science Foundation Judith Jackson, Director, Office of Communication, Fermi National Accelerator Laboratory Young-Kee Kim, Deputy Director, Fermi National Accelerator Laboratory John Kogut, HEPAP Executive Secretary, Office of High Energy Physics, Office of Science, Department of Energy Dennis Kovar, Associate Director, Office of High Energy Physics, Office of Science, Department of Energy Kevin Lesko, Nuclear Science Division, Lawrence Berkeley National Laboratory Marsha Marsden, Office of High Energy Physics, Office of Science, -
January 26, 2009
INFORMATION Texting, blogging and the like might yet prove beneficial, 3 BIOLOGICAL SCIENCE Avian dads learned doting ways from the dinosaurs, 4 CENTER FOR TEACHING AND LEARNING Lectures, workshops and The Faculty-Staff Bulletin of The Florida State University consultations, 6 and 7 VolumeSTATE 43 • Number 10 January 26 - February 15, 2009 Florida State pays tribute to ‘Year of Science’ ORIGINS ’09 Two-time Pulitzer Prize-winning au- Wilson will join acclaimed Harvard NPR’s “Science Friday,” among many thor and world-renowned biologist E.O. University cosmologist Lisa Randall, others for the program, which begins Wilson will be among the headliners of famed anthropologist Don Johanson (co- March 16. a two-week celebration of what discov- discoverer of “Lucy”, the world’s most Named “Origins ’09: A Celebration eries in science and the humanities have famous fossil), Sean B. Carroll, noted of the Birth and Life of Beginnings,” the meant to modern civilization. biologist and author, and Ira Flatow of event is being sponsored by the Florida State University Office of Research and co-sponsored by the FSU College of Medicine and the Tallahassee Scientific Conference headliners will Society. It’s all part of a tribute to 2009 include, clockwise, E.O. as the Year of Science, a national desig- Wilson, the world’s leading nation inspired by the 200th birthday of Charles Darwin (Feb. 12). naturalist, Harvard physicist Unlike many tributes scheduled Lisa Randall and Ira Flatow, around the nation and world, Florida host of “Science Friday” on State’s program is designed to go be- National Public Radio. -
Curriculum Vitae
CURRICULUM VITAE Raman Sundrum July 26, 2019 CONTACT INFORMATION Physical Sciences Complex, University of Maryland, College Park, MD 20742 Office - (301) 405-6012 Email: [email protected] CAREER John S. Toll Chair, Director of the Maryland Center for Fundamental Physics, 2012 - present. Distinguished University Professor, University of Maryland, 2011-present. Elkins Chair, Professor of Physics, University of Maryland, 2010-2012. Alumni Centennial Chair, Johns Hopkins University, 2006- 2010. Full Professor at the Department of Physics and Astronomy, The Johns Hopkins University, 2001- 2010. Associate Professor at the Department of Physics and Astronomy, The Johns Hop- kins University, 2000- 2001. Research Associate at the Department of Physics, Stanford University, 1999- 2000. Advisor { Prof. Savas Dimopoulos. 1 Postdoctoral Fellow at the Department of Physics, Boston University. 1996- 1999. Postdoc advisor { Prof. Sekhar Chivukula. Postdoctoral Fellow in Theoretical Physics at Harvard University, 1993-1996. Post- doc advisor { Prof. Howard Georgi. Postdoctoral Fellow in Theoretical Physics at the University of California at Berke- ley, 1990-1993. Postdoc advisor { Prof. Stanley Mandelstam. EDUCATION Yale University, New-Haven, Connecticut Ph.D. in Elementary Particle Theory, May 1990 Thesis Title: `Theoretical and Phenomenological Aspects of Effective Gauge Theo- ries' Thesis advisor: Prof. Lawrence Krauss Brown University, Providence, Rhode Island Participant in the 1988 Theoretical Advanced Summer Institute University of Sydney, Australia B.Sc with First Class Honours in Mathematics and Physics, Dec. 1984 AWARDS, DISTINCTIONS J. J. Sakurai Prize in Theoretical Particle Physics, American Physical Society, 2019. Distinguished Visiting Research Chair, Perimeter Institute, 2012 - present. 2 Moore Fellow, Cal Tech, 2015. American Association for the Advancement of Science, Fellow, 2011. -
Supergravity on the Brane
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Supergravity on the Brane A. Chamblin∗∗ & G.W. Gibbons DAMTP, Silver Street, Cambridge, CB3 9EW, England (November 23, 1999) We show that smooth domain wall spacetimes supported by a scalar field separating two anti- de-Sitter like regions admit a single graviton bound state. Our analysis yields a fully non-linear supergravity treatment of the Randall-Sundrum model. Our solutions describe a pp-wave propa- gating in the domain wall background spacetime. If the latter is BPS, our solutions retain some supersymmetry. Nevertheless, the Kaluza-Klein modes generate \pp curvature" singularities in the bulk located where the horizon of AdS would ordinarily be. 12.10.-g, 11.10.Kk, 11.25.M, 04.50.+h DAMTP-1999-126 I. INTRODUCTION full dynamics of the domain wall is not treated in detail in the Randall-Sundrum model. In fact gravitating domain walls have a drastic effect on the curvature of the ambi- It has long been thought that any attempt to model ent spacetime and it is not obvious that a simple model the Universe as a single brane embedded in a higher- involving a single collective coordinate representing the dimensional bulk spacetime must inevitably fail because transverse displacement of the domain wall is valid. the gravitational forces experienced by matter on the For these reasons it seems desirable to have a simple brane, being mediated by gravitons travelling in the non-singular model which is exactly solvable. It is the bulk, are those appropriate to the higher dimensional purpose of this note to provide that. -
Axion Dark Matter from Higgs Inflation with an Intermediate H∗
Axion dark matter from Higgs inflation with an intermediate H∗ Tommi Tenkanena and Luca Visinellib;c;d aDepartment of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA bDepartment of Physics and Astronomy, Uppsala University, L¨agerhyddsv¨agen1, 75120 Uppsala, Sweden cNordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, 10691 Stockholm, Sweden dGravitation Astroparticle Physics Amsterdam (GRAPPA), Institute for Theoretical Physics Amsterdam and Delta Institute for Theoretical Physics, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands E-mail: [email protected], [email protected], [email protected] Abstract. In order to accommodate the QCD axion as the dark matter (DM) in a model in which the Peccei-Quinn (PQ) symmetry is broken before the end of inflation, a relatively low scale of inflation has to be invoked in order to avoid bounds from DM isocurvature 9 fluctuations, H∗ . O(10 ) GeV. We construct a simple model in which the Standard Model Higgs field is non-minimally coupled to Palatini gravity and acts as the inflaton, leading to a 8 scale of inflation H∗ ∼ 10 GeV. When the energy scale at which the PQ symmetry breaks is much larger than the scale of inflation, we find that in this scenario the required axion mass for which the axion constitutes all DM is m0 . 0:05 µeV for a quartic Higgs self-coupling 14 λφ = 0:1, which correspond to the PQ breaking scale vσ & 10 GeV and tensor-to-scalar ratio r ∼ 10−12. Future experiments sensitive to the relevant QCD axion mass scale can therefore shed light on the physics of the Universe before the end of inflation. -
Modified Newtonian Dynamics, an Introductory Review
Modified Newtonian Dynamics, an Introductory Review Riccardo Scarpa European Southern Observatory, Chile E-mail [email protected] Abstract. By the time, in 1937, the Swiss astronomer Zwicky measured the velocity dispersion of the Coma cluster of galaxies, astronomers somehow got acquainted with the idea that the universe is filled by some kind of dark matter. After almost a century of investigations, we have learned two things about dark matter, (i) it has to be non-baryonic -- that is, made of something new that interact with normal matter only by gravitation-- and, (ii) that its effects are observed in -8 -2 stellar systems when and only when their internal acceleration of gravity falls below a fix value a0=1.2×10 cm s . Being completely decoupled dark and normal matter can mix in any ratio to form the objects we see in the universe, and indeed observations show the relative content of dark matter to vary dramatically from object to object. This is in open contrast with point (ii). In fact, there is no reason why normal and dark matter should conspire to mix in just the right way for the mass discrepancy to appear always below a fixed acceleration. This systematic, more than anything else, tells us we might be facing a failure of the law of gravity in the weak field limit rather then the effects of dark matter. Thus, in an attempt to avoid the need for dark matter many modifications of the law of gravity have been proposed in the past decades. The most successful – and the only one that survived observational tests -- is the Modified Newtonian Dynamics.