The Bose-Einstein Condensate and Cold Atom Laboratory
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Companion Q&A Fact Sheet: What Mars Reveals About Life in Our
What Mars Reveals about Life in Our Universe Companion Q&A Fact Sheet Educators from the Smithsonian’s Air and Space and Natural History Museums assembled this collection of commonly asked questions about Mars to complement the Smithsonian Science How webinar broadcast on March 3, 2021, “What Mars Reveals about Life in our Universe.” Continue to explore Mars and your own curiosities with these facts and additional resources: • NASA: Mars Overview • NASA: Mars Robotic Missions • National Air and Space Museum on the Smithsonian Learning Lab: “Wondering About Astronomy Together” Guide • National Museum of Natural History: A collection of resources for teaching about Antarctic Meteorites and Mars 1 • Smithsonian Science How: “What Mars Reveals about Life in our Universe” with experts Cari Corrigan, L. Miché Aaron, and Mariah Baker (aired March 3, 2021) Mars Overview How long is Mars’ day? Mars takes 24 hours and 38 minutes to spin around once, so its day is very similar to Earth’s. How long is Mars’ year? Mars takes 687 days, almost two Earth years, to complete one orbit around the Sun. How far is Mars from Earth? The distance between Earth and Mars changes as both planets move around the Sun in their orbits. At its closest, Mars is just 34 million miles from the Earth; that’s about one third of Earth’s distance from the Sun. On the day of this program, March 3, 2021, Mars was about 135 million miles away, or four times its closest distance. How far is Mars from the Sun? Mars orbits an average of 141 million miles from the Sun, which is about one-and-a-half times as far as the Earth is from the Sun. -
Physical Changes
How Matter Changes By Cindy Grigg Changes in matter happen around you every day. Some changes make matter look different. Other changes make one kind of matter become another kind of matter. When you scrunch a sheet of paper up into a ball, it is still paper. It only changed shape. You can cut a large, rectangular piece of paper into many small triangles. It changed shape and size, but it is still paper. These kinds of changes are called physical changes. Physical changes are changes in the way matter looks. Changes in size and shape, like the changes in the cut pieces of paper, are physical changes. Physical changes are changes in the size, shape, state, or appearance of matter. Another kind of physical change happens when matter changes from one state to another state. When water freezes and makes ice, it is still water. It has only changed its state of matter from a liquid to a solid. It has changed its appearance and shape, but it is still water. You can change the ice back into water by letting it melt. Matter looks different when it changes states, but it stays the same kind of matter. Solids like ice can change into liquids. Heat speeds up the moving particles in ice. The particles move apart. Heat melts ice and changes it to liquid water. Metals can be changed from a solid to a liquid state also. Metals must be heated to a high temperature to melt. Melting is changing from a solid state to a liquid state. -
Cosmic Microwave Background
1 29. Cosmic Microwave Background 29. Cosmic Microwave Background Revised August 2019 by D. Scott (U. of British Columbia) and G.F. Smoot (HKUST; Paris U.; UC Berkeley; LBNL). 29.1 Introduction The energy content in electromagnetic radiation from beyond our Galaxy is dominated by the cosmic microwave background (CMB), discovered in 1965 [1]. The spectrum of the CMB is well described by a blackbody function with T = 2.7255 K. This spectral form is a main supporting pillar of the hot Big Bang model for the Universe. The lack of any observed deviations from a 7 blackbody spectrum constrains physical processes over cosmic history at redshifts z ∼< 10 (see earlier versions of this review). Currently the key CMB observable is the angular variation in temperature (or intensity) corre- lations, and to a growing extent polarization [2–4]. Since the first detection of these anisotropies by the Cosmic Background Explorer (COBE) satellite [5], there has been intense activity to map the sky at increasing levels of sensitivity and angular resolution by ground-based and balloon-borne measurements. These were joined in 2003 by the first results from NASA’s Wilkinson Microwave Anisotropy Probe (WMAP)[6], which were improved upon by analyses of data added every 2 years, culminating in the 9-year results [7]. In 2013 we had the first results [8] from the third generation CMB satellite, ESA’s Planck mission [9,10], which were enhanced by results from the 2015 Planck data release [11, 12], and then the final 2018 Planck data release [13, 14]. Additionally, CMB an- isotropies have been extended to smaller angular scales by ground-based experiments, particularly the Atacama Cosmology Telescope (ACT) [15] and the South Pole Telescope (SPT) [16]. -
Quantum Reflection in Two Dimensions
Quantum Reflection in Two Dimensions Emanuele Galiffi Department of Physics Imperial College London - University of Heidelberg This dissertation is submitted for the degree of MSci Physics Imperial College London July 2015 University of Heidelberg To my family: Francesco, Mariangela and Davide. Declaration This project is embedded in a larger project with a long-term perspective in the numerical study of quantum reflection (QR) in atom-surface scattering problems. The project leaders are Sandro Wimberger (University of Parma, University of Heidelberg) and Dr. Maarten DeKieviet (University of Heidelberg). The first project, which was carried out by B. Herwerth, concerned the development and implementation of numerical time-dependent methods used in 1D studies. These found an application in the study of QR off vibrating surfaces. In the second project, which was carried out by Sünderhauf, different approaches to 2D wavepacket propagation were considered from a general point of view. The computational costs associated to the matrix decomposition of the 2D Hamiltonian matrix were estimated in that context. Furthermore, comparisons were drawn between quantum and classical reflection, and methods for isolating the two effects were investigated. Moreover, part of the 1D Fortran code written by Herwerth was translated by Sünderhauf in C++. I hereby declare that except where specific reference is made to the work of others, the contents of this dissertation are original and have not been submitted in whole or in part for consideration for any other degree or qualification in this, or any other university. This dissertation is my own work and contains nothing which is the outcome of work done in collaboration with others, except as specified in the text and Acknowledgements. -
The Temperature of the Cosmic Microwave Background at 10 Ghz D
The Astrophysical Journal, 612:86–95, 2004 September 1 # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE TEMPERATURE OF THE COSMIC MICROWAVE BACKGROUND AT 10 GHZ D. J. Fixsen,1 A. Kogut,2 S. Levin,3 M. Limon,1 P. Lubin,4 P. Mirel,1 M. Seiffert,3 and E. Wollack2 Received 2004 February 23; accepted 2004 April 14 ABSTRACT We report the results of an effort to measure the low-frequency portion of the spectrum of the cosmic microwave background (CMB) radiation, using a balloon-borne instrument called the Absolute Radiometer for Cosmology, Astrophysics, and Diffuse Emission (ARCADE). These measurements are to search for deviations from a thermal spectrum that are expected to exist in the CMB as a result of various processes in the early universe. The radiometric temperature was measured at 10 and 30 GHz using a cryogenic open-aperture instrument with no emissive windows. An external blackbody calibrator provides an in situ reference. Systematic errors were greatly reduced by using differential radiometers and cooling all critical components to physical temperatures approxi- mating the antenna temperature of the sky. A linear model is used to compare the radiometer output to a set of thermometers on the instrument. The unmodeled residualsarelessthan50mKpeaktopeakwithaweightedrms of 6 mK. Small corrections are made for the residual emission from the flight train, atmosphere, and foreground Galactic emission. The measured radiometric temperature of the CMB is 2:721 Æ 0:010 K at 10 GHz and 2:694 Æ 0:032 K at 30 GHz. Subject headinggs: cosmic microwave background — cosmology: observations 1. -
Extreme Cold Is a Dangerous Situation That Can Bring on Bring Can That Situation Dangerous a Is Cold Extreme
Centers for Disease Control and Prevention and Control Disease for Centers U.S. Department of Health And Human Services Human And Health of Department U.S. U.S. Department of Health And Human Services Centers for Disease Control and Prevention http://www.bt.cdc.gov/disasters/winter/ 1-888-232-6789; [email protected] 1-888-232-6789; 4700 Buford Hwy, Atlanta, GA 30341-3717 GA Atlanta, Hwy, Buford 4700 National Center for Environmental Health, MS F52 MS Health, Environmental for Center National Centers for Disease Control and Prevention and Control Disease for Centers or more information on cold weather conditions and health, please contact: please health, and conditions weather cold on information more or F For more information on hot weather conditions and health, please contact: Centers for Disease Control and Prevention National Center for Environmental Health, MS F52 4700 Buford Hwy, Atlanta, GA 30341-3717 1-888-232-6789; [email protected] http://www.bt.cdc.gov/disasters/extremeheat/ 1 and what to do if a cold-weather health emergency arises. arises. emergency health cold-weather a if do to what and should know how to prevent cold-related health problems health cold-related prevent to how know should that is poorly insulated or without heat. without or insulated poorly is that can be affected. To keep yourself and your family safe, you safe, family your and yourself keep To affected. be can without shelter or who are stranded, or who live in a home a in live who or stranded, are who or shelter without Infants and the elderly are particularly at risk, but anyone but risk, at particularly are elderly the and Infants health emergencies in susceptible people, such as those as such people, susceptible in emergencies health can cause other serious or life-threatening health problems. -
Cold-To-Warm Flow Regime Transition in Snow Avalanches
Cold-to-warm flow regime transition in snow avalanches Köhler Anselm1,2, Fischer Jan-Thomas2, Scandroglio Riccardo1, Bavay Mathias1, McElwaine Jim3, and Sovilla Betty1 1WSL Institute for Snow and Avalanche Research SLF, Davos Dorf, Switzerland 2Austrian Research Centre for Forests (BFW), Innsbruck, Austria 3Department of Earth Sciences, Durham University, Durham, UK Correspondence to: Anselm Köhler, [email protected] Abstract. Large avalanches usually encounter different snow conditions along their track. When they release as slab avalanches comprising cold snow, they can subsequently develop into powder snow avalanches entraining snow as they move down the mountain. Typically, this entrained snow will be cold (T < −1 ◦C) at high elevations near the surface, but warm (T > −1 ◦C) at lower elevations or deeper in the snow pack. The intake of warm snow is believed to be of major importance to increase the 5 temperature of the snow composition in the avalanche and eventually cause a flow regime transition. Measurements of flow regime transitions are performed at the Vallée de la Sionne avalanche test site in Switzerland using two different radar systems. The data are then combined with snow temperatures calculated with the snow cover model SNOWPACK. We define transitions as complete, when the deposit at runout is characterized only by warm snow, or as partial, if there is a warm flow regime but the farthest deposit is characterized by cold snow. We introduce a transition index Ft, based on the runout of cold and warm flow 10 regimes, as a measure to quantify the transition type. Finally, we parameterize the snow cover temperature along the avalanche track by the altitude Hs, which represents the point where the average temperature of the uppermost 0:5 m changes from cold to warm. -
Absolute Zero Summative Evaluation
Absolute Zero Summative Evaluation PREPARED BY Marianne McPherson, M.S., M.A. Laura Houseman Irene F. Goodman, Ed.D. SUBMITTED TO Meredith Burch, Meridian Productions, Inc. Linda Devillier, Devillier Communications, Inc. Professor Russell Donnelly, University of Oregon October 2008 GOODMAN RESEARCH GROUP, INC. August 2003 1 ACKNOWLEDGMENTS GRG acknowledges the following individuals for their contributions to the Absolute Zero summative evaluation: • Professor Russell Donnelly at the University of Oregon, Linda Devillier of Devillier Communications, Inc., and Meredith Burch of Meridian Productions Inc. for their supportive collaboration; • GRG assistants Nina Grant, Stephanie Lewis, Theresa Rowley, and Zoe Shei for data entry and coordination of the evaluation of outreach materials; • The adult and student viewers who participated in the evaluation of the television series, and the teachers who evaluated the outreach materials; • The National Partners, Participants, and Absolute Zero Experts who participated in the survey and interviews. This report was written under contract to University of Oregon, National Science Foundation grant # 0307939. The views expressed are solely those of Goodman Research Group, Inc. GOODMAN RESEARCH GROUP, INC. October 2008 TABLE OF CONTENTS Executive Summary......................................................................................... i Introduction..................................................................................................... 1 Methods ......................................................................................................... -
Arctic and Antarctic Research
Science on the Edge arctic and antarctic discoveries he polar regions provide unique natural laboratories for the study of Tcomplex scientific questions, ranging from human origins in the New World to the expansion of the universe. People have studied the polar regions for centuries. The extreme cold and stark beauty of the Arctic and Antarctic capture the imaginations of explorers, naturalists, and armchair travelers. In the latter half of the twentieth century, NSF-funded scientists discovered that the Arctic and the Antarctic have much to teach us about our Earth and its atmosphere, oceans, and climate. For example, cores drilled from the great ice sheets of Greenland and Antarctica tell a story of global climate changes throughout history. During NSF’s lifetime, the extreme environments of the Arctic and Antarctic have become learning environments. During the First Polar Year (1882–83), scien- tists and explorers journeyed to the icy margins of the Earth to collect data on weather patterns, the Earth’s magnetic force, and other polar phe- nomena that affected navigation and shipping in A Surprising Abundance of Life the era of expanding commerce and industrial Both the Arctic and Antarctic seem beyond life: development. In all, the First Polar Year inspired icy, treeless, hostile places. Yet these polar regions fifteen expeditions (twelve to the Arctic and three host a surprising abundance of life, ranging from to the Antarctic) by eleven nations. Along the way, the microbial to the awe-inspiring, from bacteria researchers established twelve research stations. to bowhead whales. By the Second Polar Year (1932–33), new fields The United States has supported research Important differences mark North and South. -
Thermodynamic Temperature
Thermodynamic temperature Thermodynamic temperature is the absolute measure 1 Overview of temperature and is one of the principal parameters of thermodynamics. Temperature is a measure of the random submicroscopic Thermodynamic temperature is defined by the third law motions and vibrations of the particle constituents of of thermodynamics in which the theoretically lowest tem- matter. These motions comprise the internal energy of perature is the null or zero point. At this point, absolute a substance. More specifically, the thermodynamic tem- zero, the particle constituents of matter have minimal perature of any bulk quantity of matter is the measure motion and can become no colder.[1][2] In the quantum- of the average kinetic energy per classical (i.e., non- mechanical description, matter at absolute zero is in its quantum) degree of freedom of its constituent particles. ground state, which is its state of lowest energy. Thermo- “Translational motions” are almost always in the classical dynamic temperature is often also called absolute tem- regime. Translational motions are ordinary, whole-body perature, for two reasons: one, proposed by Kelvin, that movements in three-dimensional space in which particles it does not depend on the properties of a particular mate- move about and exchange energy in collisions. Figure 1 rial; two that it refers to an absolute zero according to the below shows translational motion in gases; Figure 4 be- properties of the ideal gas. low shows translational motion in solids. Thermodynamic temperature’s null point, absolute zero, is the temperature The International System of Units specifies a particular at which the particle constituents of matter are as close as scale for thermodynamic temperature. -
Quantum Reflection from the Casimir-Polder Potential
THÈSE DE DOCTORAT DE L’UNIVERSITÉ PIERRE ET MARIE CURIE Spécialité : Physique École doctorale : “Physique en Île-de-France” réalisée au Laboratoire Kastler-Brossel présentée par Gabriel DUFOUR pour obtenir le grade de DOCTEUR DE L’UNIVERSITÉ PIERRE ET MARIE CURIE Sujet de la thèse : Réflexion quantique sur le potentiel de Casimir-Polder – Quantum reflection from the Casimir-Polder potential soutenue le 20 novembre 2015 devant le jury composé de M Andreas Buchleitner Rapporteur M David Guéry-Odelin Rapporteur Mme Marie-Christine Angonin Examinatrice M Olivier Dulieu Examinateur M Valery Nesvizhevsky Examinateur Mme Astrid Lambrecht Directrice de thèse i À la mémoire de mes grands-pères, Jean Dufour et Michel Durin ii Quand j’ai poussé la porte du Laboratoire Kastler Brossel en novembre 2011, je re- venais d’un mois de voyage à vélo sur les routes et chemins d’Italie. Astrid Lambrecht et Serge Reynaud m’ont convaincu de me lancer dans une nouvelle aventure, avec son lot d’ascensions ardues, de petites victoires, de problèmes techniques et de découvertes grisantes. Astrid et Serge m’ont accompagné sans relâche au cours du stage et de la thèse qui ont suivi. Je les remercie chaleureusement pour leur gentillesse et leur patience, leurs mots d’encouragement et les nombreuses discussions passionnantes que nous avons eues. Marie-Pascale Gorza, Romain Guérout, Manuel Donaire et Axel Maury ont été mes compagnons de route au sein de l’équipe “fluctuations quantiques et relativité”. Leurs conversations stimulantes et animées ont égayé bien des austères journées de travail. J’ai aussi partagé de très bons moments avec mes collègues et amis du laboratoire et d’au delà, que ce soit dans les courants d’air de la cantine, sous le soleil des arènes ou dans l’ambiance chaleureuse d’une cafétéria. -
Mars Activities
MARS ACTIVITIES Teacher Resources and Classroom Activities Mars Education Program Jet Propulsion Laboratory Arizona State University Mars Missions Information and Updates Mission Information Available at Jet Propulsion Laboratory Mars Exploration Home Page http://mars.jpl.nasa.gov More Educational Activities Available at Jet Propulsion Laboratory Mars Education & Public Outreach Program http://mars.jpl.nasa.gov/classroom or Arizona State University Mars K-12 Education Program http://tes.asu.edu/neweducation.html Table of Contents 1. Earth, Moon, Mars Balloons 1 2. Rover Races 4 3. Areology - The Study of Mars 11 4. Strange New Planet 16 5. Lava Layering 24 6. Searching for Life on Mars 33 7. Mars Critters 42 8. Exploring Crustal Material from a Mystery Planet 46 - Graph Paper 48 9. Edible Mars Rover 49 - Mars Pathfinder Rover 51 10. Edible Mars Spacecraft 52 - Mars Global Surveyor 54 - Mars Pathfinder 55 - Mars Pathfinder Rover 56 11. Mars Meteorites’ Fingerprints 57 12. Introduction to Creating a Mission Plan 65 13. Out of Sight: Remote Vehicle Activity 66 - Mars Rover Websites 69 15. Probing Below the Surface of Mars 74 16. Good Vibrations 85 17. The Mathematics of Mars 90 - “I Have…Who Has?” Cards 93 18. Mars Bingo 100 19. Mud Splat Craters 112 20. Solar System Beads Distance Activity 115 21. Alka-Seltzer Rockets 118 22. Soda Straw Rockets 122 23. Mars Pathfinder: Two-Dimensional Model 126 24. Mars Pathfinder: Egg Drop and Landing 127 25. Cool Internet Sites 128 Earth, Moon, Mars Balloons 1 Introduction: How big is the Moon; how far is it relative to Earth? Earth science and astronomy books depict a moon that is much closer and much larger than in reality.