DSU2010 the Dark Side of the Universe 2010
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Emerging Issues in Cosmology & Particle Physics
Organizing Committee Patron Principal, Siksha Bhavana, Visva-Bharati Conveners Swarup Kumar Majee & Biswajit Pandey Program Advisory Committee AJIT KEMBHAVI, IUCAA, India AJIT SRIVASTAVA, IOPB , India International Conference on ALAKABHA DATTA, Univ. of Mississippi, USA AMITAVA RAYCHAUDHURI, Univ. Of Calcutta, India AMOL DIGHE, TIFR, India Emerging Issues ASANTHA R. COORAY, UC-Irvine, USA BISWARUP MUKHOPADHYAYA, HRI, India CHENG-WEI CHIANG, NTU, Taiwan in DIEGO PAVON, AUB, Spain EUNG JIN CHUN, KIAS, South Korea GORAN SENJANOVIC, INFN, Italy Cosmology & KAI-FENG CHEN, NTU, Taiwan NABA KUMAR MONDAL, SINP, India NOBUCHIKA OKADA, Univ. of Alabama, USA Particle Physics Organized by QAISAR SHAFI, Univ. of Delaware, USA RABINDRA MOHAPATRA, Univ. of Maryland, USA Department of Physics, RENNAN BARKANA, Tel Aviv University, Israel January 12 -14, 2020 SOMAK RAYCHAUDHURY, IUCAA, India VISVA-BHARATI UNIVERSITY SOMNATH BHARADWAJ, IIT, Kharagpur, India Visva-Bharati University THOMAS BUCHERT, CRAL, Univ. of Lyon, France Santiniketan Email: [email protected] UTPAL SARKAR, IIT, Kharagpur, India Mob.: (+91) 7908272177/ 7602198961 / 8972889271 VOLKER SPRINGEL, MPA, Garching, Germany India Conference webpage: https://indico.cern.ch/event/849205/ Local Organizing Committee Registration Fee Details All faculty members of the Department Indian participants Foreign participants of Physics, Visva-Bharati university Faculty Members INR 4000 USD 200 Ph.D. Students/ Postdocs INR 2000 USD 100 Conference Topics Undergraduate/M.Sc. Students INR 500 USD 75 The registration fee will cover registration kits, refreshments, lunch, dinner, conference dinner and Dark Matter & Dark Energy local transportation. Neutrino Physics Accelerator Physics The main objective of the conference is to provide a common platform to discuss the emerging issues Physics Beyond the Standard Model in cosmology and particle physics, to set out possible future collaborative research works and to nail 21 cm Cosmology down some existing common problems. -
Book of Abstracts
The 19th Particles and Nuclei International Conference (PANIC11) Scientific Program Laboratory for Nuclear Science Massachusetts Institute of Technology July 24-29, 2011 Table of Contents Contents Sunday, 24 July 1 Pedagogical Lectures for Students - Kresge Auditorium (09:00-15:45)................. 1 Welcome Reception - Kresge Oval Tent (16:00-19:00) . ................... 1 Monday, 25 July 2 Opening Remarks - Kresge Auditorium (08:30-08:55) . ................... 2 Plenary1 - KresgeAuditorium (08:30-10:05) . ................. 2 Plenary1 - KresgeAuditorium (10:45-12:00) . ................. 2 Parallel 1A - Parity Violating Scattering - W20-307 (MezzanineLounge)(13:30-15:30) . 3 Parallel 1B - Nuclear Effects & Hadronization - W20-306 (20 Chimneys)(13:30-15:30) . 4 Parallel 1C - Recent Baryon Results I - W20-201 (West Lounge) (13:30-15:30). 6 Parallel 1D - Kaonic Atoms and Hypernuclear Physics - 4-149 (13:30-15:30) . 8 Parallel 1E - Neutrino Oscillations I - 4-163 (13:30-15:30) ....................... 10 Parallel 1F - Dark Forces and Dark Matter - 4-153 (13:30-15:30) ................... 12 Parallel 1G - P- and T-violating weak decays - Kresge - RehearsalA(13:30-15:30) . 14 Parallel 1H - Electroweak Cross Sections at the TeV Scale - Kresge - Rehearsal B (13:30-15:30) . 16 Parallel 1I - CKM & CP Violation - Kresge - Little Theatre (13:30-15:30) .............. 17 Parallel 1J - Collider Searches Beyond the Standard Model - Kresge Auditorium (13:30-15:30) . 18 Parallel 1K - Hydrodynamics - W20-407 (13:30-15:30) . ................... 19 Parallel 1L - Heavy Ion Collisions I - W20-491 (13:30-15:30) ...................... 20 Parallel 2A - Generalized Parton Distributions - W20-307 (Mezzanine Lounge) (16:00-17:40). 21 Parallel 2B - Parton Distribution Functions and Fits - W20-306 (20 Chimneys) (16:00-17:40) . -
Table of Contents (Print)
PERIODICALS PHYSICAL REVIEW Dä For editorial and subscription correspondence, Postmaster send address changes to: please see inside front cover (ISSN: 1550-7998) APS Subscription Services P.O. Box 41 Annapolis Junction, MD 20701 THIRD SERIES, VOLUME 90, NUMBER 5 CONTENTS D1 SEPTEMBER 2014 RAPID COMMUNICATIONS Measurement of the electric charge of the top quark in tt¯ events (8 pages) ........................................................ 051101(R) V. M. Abazov et al. (D0 Collaboration) BRST-symmetry breaking and Bose-ghost propagator in lattice minimal Landau gauge (5 pages) ............................. 051501(R) Attilio Cucchieri, David Dudal, Tereza Mendes, and Nele Vandersickel ARTICLES pffiffiffi Search for supersymmetry in events with four or more leptons in s ¼ 8 TeV pp collisions with the ATLAS detector (33 pages) ................................................................................................................................. 052001 G. Aad et al. (ATLAS Collaboration) pffiffiffi Low-mass vector-meson production at forward rapidity in p þ p collisions at s ¼ 200 GeV (12 pages) .................. 052002 A. Adare et al. (PHENIX Collaboration) Measurement of Collins asymmetries in inclusive production of charged pion pairs in eþe− annihilation at BABAR (26 pages) 052003 J. P. Lees et al. (BABAR Collaboration) Measurement of the Higgs boson mass from the H → γγ and H → ZZÃ → 4l channels in pp collisions at center-of-mass energies of 7 and 8 TeV with the ATLAS detector (35 pages) ................................................................... 052004 G. Aad et al. (ATLAS Collaboration) pffiffiffi Search for high-mass dilepton resonances in pp collisions at s ¼ 8 TeV with the ATLAS detector (30 pages) .......... 052005 G. Aad et al. (ATLAS Collaboration) Search for low-mass dark matter with CsI(Tl) crystal detectors (6 pages) .......................................................... 052006 H. -
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. -
Tests of Chameleon Gravity
Tests of Chameleon Gravity Clare Burrage,a;∗ and Jeremy Saksteinb;y aSchool of Physics and Astronomy University of Nottingham, Nottingham, NG7 2RD, UK bCenter for Particle Cosmology, Department of Physics and Astronomy University of Pennsylvania, Philadelphia, PA 19104, USA Abstract Theories of modified gravity where light scalars with non-trivial self-interactions and non-minimal couplings to matter|chameleon and symmetron theories|dynamically sup- press deviations from general relativity in the solar system. On other scales, the environ- mental nature of the screening means that such scalars may be relevant. The highly- nonlinear nature of screening mechanisms means that they evade classical fifth-force searches, and there has been an intense effort towards designing new and novel tests to probe them, both in the laboratory and using astrophysical objects, and by reinter- preting existing datasets. The results of these searches are often presented using different parametrizations, which can make it difficult to compare constraints coming from dif- ferent probes. The purpose of this review is to summarize the present state-of-the-art searches for screened scalars coupled to matter, and to translate the current bounds into a single parametrization to survey the state of the models. Presently, commonly studied chameleon models are well-constrained but less commonly studied models have large re- gions of parameter space that are still viable. Symmetron models are constrained well by astrophysical and laboratory tests, but there is a desert separating the two scales where the model is unconstrained. The coupling of chameleons to photons is tightly constrained but the symmetron coupling has yet to be explored. -
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. -
![Arxiv:1906.00969V2 [Hep-Ph] 2 Sep 2019](https://docslib.b-cdn.net/cover/1333/arxiv-1906-00969v2-hep-ph-2-sep-2019-601333.webp)
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]. -
![Arxiv:1603.06587V1 [Astro-Ph.CO] 21 Mar 2016 Nevertheless They Have Managed to Escape Detection (Thus Far) Through So-Called Screening Mech- Anisms](https://docslib.b-cdn.net/cover/9632/arxiv-1603-06587v1-astro-ph-co-21-mar-2016-nevertheless-they-have-managed-to-escape-detection-thus-far-through-so-called-screening-mech-anisms-909632.webp)
Arxiv:1603.06587V1 [Astro-Ph.CO] 21 Mar 2016 Nevertheless They Have Managed to Escape Detection (Thus Far) Through So-Called Screening Mech- Anisms
Chameleon Dark Energy and Atom Interferometry Benjamin Elder1, Justin Khoury1, Philipp Haslinger3, Matt Jaffe3, Holger M¨uller3;4, Paul Hamilton2 1Center for Particle Cosmology, Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104 2Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 3Department of Physics, University of California, Berkeley, CA 94720 4Lawrence Berkeley National Laboratory, Berkeley, CA, 94720 Abstract Atom interferometry experiments are searching for evidence of chameleon scalar fields with ever-increasing precision. As experiments become more precise, so too must theoretical predictions. Previous work has made numerous approximations to simplify the calculation, which in general requires solving a 3-dimensional nonlinear partial differential equation (PDE). In this paper, we introduce a new technique for calculating the chameleonic force, using a numerical relaxation scheme on a uniform grid. This technique is more general than previous work, which assumed spherical symmetry to reduce the PDE to a 1-dimensional ordinary differential equation (ODE). We examine the effects of approximations made in previous efforts on this subject, and calculate the chameleonic force in a set-up that closely mimics the recent experiment of Hamilton et al. Specifically, we simulate the vacuum chamber as a cylinder with dimensions matching those of the experiment, taking into account the backreaction of the source mass, its offset from the center, and the effects of the chamber walls. Remarkably, the acceleration on a test atomic particle is found to differ by only 20% from the approximate analytical treatment. These results allow us to place rigorous constraints on the parameter space of chameleon field theories, although ultimately the constraint we find is the same as the one we reported in Hamilton et al. -
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. -
Qaisar Shafi Studied for His B
Qaisar Shafi received his BSc and his PhD in Theoretical Physics from Imperial College, London. England. His PhD advisor was the late Abdus Salam who received the Nobel Prize for Theoretical Physics in 1979. After completing his PhD, Professor Shafi held prestigious postdoctoral and research fellowships including an Alexander von Humboldt fellowship at the Universities of Munich and Aachen, Germany, and a senior fellowship at CERN in Geneva, Switzerland. He also completed his Habilitation with venia legendi at the University of Freiburg, Germany. He joined the Bartol Research Institute at the University of Delaware in 1983. Throughout his career at the University of Delaware, Professor Shafi has maintained close ties to the ICTP (International Center for Theoretical Physics) in Trieste, Italy where he directed more than a dozen summer schools in High Energy Physics and Cosmology. He also (co-)directed a NATO school and several summer schools in High Energy Physics organized under BCSVPIN (an acronym denoting the countries Bangladesh, China, Sri Lanka, Vietnam, Pakistan, and India), an international science network, founded in collaboration with Abdus Salam and Jogesh Pati, and continued by Professor Shafi. Qaisar Shafi is an internationally recognized expert in Elementary Particle (High Energy) Physics and Cosmology; his current research areas include Higgs boson, supersymmetry, new physics at the LHC, dark matter particle, inflationary cosmology and primordial gravity waves, origin of matter in the universe and nature of dark energy. Professor Shafi has supervised a large number of postdoctoral fellows and PhD students, and created a global network of collaborators. Many of his former students and postdocs have become highly respected scientists in their home countries. -
The Gammev-CHASE Search for Couplings Between Light and Chameleon Dark Energy
How Dark Is Dark Energy? The GammeV-CHASE Search for Couplings between Light and Chameleon Dark Energy Jason Steffen, FNAL; Amol Upadhye, T-2; Over the past decade, evidence has continued to mount for an astonishing astrophysical phenomenon Alan Baumbaugh, Aaron S. Chou, Peter O. Mazur, known as the cosmic acceleration. The universe appears to be expanding increasingly rapidly; distant ob- Raymond Tomlin, FNAL; A. Weltman, Cape Town; jects are receding faster and faster. If the universe consisted entirely of ordinary matter, and if gravity were William Wester, FNAL well-described by Einstein’s General Relativity, then the expansion of the universe would slow down due to attractive gravitational forces. Thus, the cosmic acceleration demands a significant change to one of our two most fundamental theories. Either General Relativity breaks down on cosmological scales, or a new type of particle must be added to the Standard Model of particle physics, the quantum theory describing all known particles. Since particle physicists have known for some time that General Relativity cannot be incorporated directly into a quantum theory such as the Standard Model, the cosmic acceleration may give some insight into a more fundamental theory unifying gravity and quantum mechanics. he simplest theoretical modification that could explain the theories consistent with current observations are “chameleon” theories, acceleration is the “cosmological constant,” a constant vacuum which “hide” fifth forces and variations in fundamental constants by Tenergy density, which Einstein noted could be added to the equations of becoming massive in high-density regions of the universe. Since massive General Relativity. The contribution of Standard Model fields to the fields give rise to very short-range forces, chameleon dark energies are cosmological constant is approximately 120 orders of magnitude greater notoriously difficult to detect. -
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.