A Table of Frequently Used Radioisotopes
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Strontium-90
EPA Facts about Strontium-90 What is strontium-90? The most common isotope of strontium is strontium-90. Radioactive strontium-90 is produced when uranium and plutonium undergo fission. Fission The time required for a radioactive substance to is the process in which the nucleus of a lose 50 percent of its radioactivity by decay is radionuclide breaks into smaller parts. Large known as the half-life. Strontium-90 has a half- amounts of radioactive strontium-90 were life of 29 years and emits beta particles of produced during atmospheric nuclear weapons relatively low energy as it decays. Yttrium-90, its tests conducted in the 1950s and 1960s. As a decay product, has a shorter half-life (64 hours) result of atmospheric testing and radioactive than strontium-90, but it emits beta particles of fallout, this strontium was dispersed and higher energy. deposited on the earth. How are people exposed to strontium- 90? What are the uses of strontium-90? Although external exposure to strontium-90 Strontium-90 is used in medical and agricultural from nuclear testing is of minor concern because studies. It is also used in thermoelectric devices environmental concentrations are low, that are built into small power supplies for use strontium in the environment can become part of the food chain. This pathway of exposure in remote locations, such as navigational beacons, remote weather stations, and space became a concern in the 1950s with the advent vehicles. Additionally, strontium-90 is used in of atmospheric testing of nuclear explosives. electron tubes, radioluminescent markers, as a With the suspension of atmospheric testing of radiation source in industrial thickness gauges, nuclear weapons, dietary intake has steadily and for treatment of eye diseases. -
NOBELIUM Element Symbol: No Atomic Number: 102
NOBELIUM Element Symbol: No Atomic Number: 102 An initiative of IYC 2011 brought to you by the RACI KERRY LAMB www.raci.org.au NOBELIUM Element symbol: No Atomic number: 102 The credit for discovering Nobelium was disputed with 3 different research teams claiming the discovery. While the first claim dates back to 1957, it was not until 1992 that the International Union of Pure and Applied Chemistry credited the discovery to a research team from Dubna in Russia for work they did in 1966. The element was named Nobelium in 1957 by the first of its claimed discoverers (the Nobel Institute in Sweden). It was named after Alfred Nobel, a Swedish chemist who invented dynamite, held more than 350 patents and bequeathed his fortune to the establishment of the Nobel Prizes. Nobelium is a synthetic element and does not occur in nature and has no known uses other than in scientific research as only tiny amounts of the element have ever been produced. Nobelium is radioactive and most likely metallic. The appearance and properties of Nobelium are unknown as insufficient amounts of the element have been produced. Nobelium is made by the bombardment of curium (Cm) with carbon nuclei. Its most stable isotope, 259No, has a half-life of 58 minutes and decays to Fermium (255Fm) through alpha decay or to Mendelevium (259Md) through electron capture. Provided by the element sponsor Freehills Patent and Trade Mark Attorneys ARTISTS DESCRIPTION I wanted to depict Alfred Nobel, the namesake of Nobelium, as a resolute young man, wearing the Laurel wreath which is the symbol of victory. -
R-Process Elements from Magnetorotational Hypernovae
r-Process elements from magnetorotational hypernovae D. Yong1,2*, C. Kobayashi3,2, G. S. Da Costa1,2, M. S. Bessell1, A. Chiti4, A. Frebel4, K. Lind5, A. D. Mackey1,2, T. Nordlander1,2, M. Asplund6, A. R. Casey7,2, A. F. Marino8, S. J. Murphy9,1 & B. P. Schmidt1 1Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia 2ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia 3Centre for Astrophysics Research, Department of Physics, Astronomy and Mathematics, University of Hertfordshire, Hatfield, AL10 9AB, UK 4Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 5Department of Astronomy, Stockholm University, AlbaNova University Center, 106 91 Stockholm, Sweden 6Max Planck Institute for Astrophysics, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany 7School of Physics and Astronomy, Monash University, VIC 3800, Australia 8Istituto NaZionale di Astrofisica - Osservatorio Astronomico di Arcetri, Largo Enrico Fermi, 5, 50125, Firenze, Italy 9School of Science, The University of New South Wales, Canberra, ACT 2600, Australia Neutron-star mergers were recently confirmed as sites of rapid-neutron-capture (r-process) nucleosynthesis1–3. However, in Galactic chemical evolution models, neutron-star mergers alone cannot reproduce the observed element abundance patterns of extremely metal-poor stars, which indicates the existence of other sites of r-process nucleosynthesis4–6. These sites may be investigated by studying the element abundance patterns of chemically primitive stars in the halo of the Milky Way, because these objects retain the nucleosynthetic signatures of the earliest generation of stars7–13. -
Nuclear Physics
Nuclear Physics Overview One of the enduring mysteries of the universe is the nature of matter—what are its basic constituents and how do they interact to form the properties we observe? The largest contribution by far to the mass of the visible matter we are familiar with comes from protons and heavier nuclei. The mission of the Nuclear Physics (NP) program is to discover, explore, and understand all forms of nuclear matter. Although the fundamental particles that compose nuclear matter—quarks and gluons—are themselves relatively well understood, exactly how they interact and combine to form the different types of matter observed in the universe today and during its evolution remains largely unknown. Nuclear physicists seek to understand not just the familiar forms of matter we see around us, but also exotic forms such as those that existed in the first moments after the Big Bang and that exist today inside neutron stars, and to understand why matter takes on the specific forms now observed in nature. Nuclear physics addresses three broad, yet tightly interrelated, scientific thrusts: Quantum Chromodynamics (QCD); Nuclei and Nuclear Astrophysics; and Fundamental Symmetries: . QCD seeks to develop a complete understanding of how the fundamental particles that compose nuclear matter, the quarks and gluons, assemble themselves into composite nuclear particles such as protons and neutrons, how nuclear forces arise between these composite particles that lead to nuclei, and how novel forms of bulk, strongly interacting matter behave, such as the quark-gluon plasma that formed in the early universe. Nuclei and Nuclear Astrophysics seeks to understand how protons and neutrons combine to form atomic nuclei, including some now being observed for the first time, and how these nuclei have arisen during the 13.8 billion years since the birth of the cosmos. -
Experimental Γ Ray Spectroscopy and Investigations of Environmental Radioactivity
Experimental γ Ray Spectroscopy and Investigations of Environmental Radioactivity BY RANDOLPH S. PETERSON 216 α Po 84 10.64h. 212 Pb 1- 415 82 0- 239 β- 01- 0 60.6m 212 1+ 1630 Bi 2+ 1513 83 α β- 2+ 787 304ns 0+ 0 212 α Po 84 Experimental γ Ray Spectroscopy and Investigations of Environmental Radioactivity Randolph S. Peterson Physics Department The University of the South Sewanee, Tennessee Published by Spectrum Techniques All Rights Reserved Copyright 1996 TABLE OF CONTENTS Page Introduction ....................................................................................................................4 Basic Gamma Spectroscopy 1. Energy Calibration ................................................................................................... 7 2. Gamma Spectra from Common Commercial Sources ........................................ 10 3. Detector Energy Resolution .................................................................................. 12 Interaction of Radiation with Matter 4. Compton Scattering............................................................................................... 14 5. Pair Production and Annihilation ........................................................................ 17 6. Absorption of Gammas by Materials ..................................................................... 19 7. X Rays ..................................................................................................................... 21 Radioactive Decay 8. Multichannel Scaling and Half-life ..................................................................... -
Chapter 3 the Fundamentals of Nuclear Physics Outline Natural
Outline Chapter 3 The Fundamentals of Nuclear • Terms: activity, half life, average life • Nuclear disintegration schemes Physics • Parent-daughter relationships Radiation Dosimetry I • Activation of isotopes Text: H.E Johns and J.R. Cunningham, The physics of radiology, 4th ed. http://www.utoledo.edu/med/depts/radther Natural radioactivity Activity • Activity – number of disintegrations per unit time; • Particles inside a nucleus are in constant motion; directly proportional to the number of atoms can escape if acquire enough energy present • Most lighter atoms with Z<82 (lead) have at least N Average one stable isotope t / ta A N N0e lifetime • All atoms with Z > 82 are radioactive and t disintegrate until a stable isotope is formed ta= 1.44 th • Artificial radioactivity: nucleus can be made A N e0.693t / th A 2t / th unstable upon bombardment with neutrons, high 0 0 Half-life energy protons, etc. • Units: Bq = 1/s, Ci=3.7x 1010 Bq Activity Activity Emitted radiation 1 Example 1 Example 1A • A prostate implant has a half-life of 17 days. • A prostate implant has a half-life of 17 days. If the What percent of the dose is delivered in the first initial dose rate is 10cGy/h, what is the total dose day? N N delivered? t /th t 2 or e Dtotal D0tavg N0 N0 A. 0.5 A. 9 0.693t 0.693t B. 2 t /th 1/17 t 2 2 0.96 B. 29 D D e th dt D h e th C. 4 total 0 0 0.693 0.693t /th 0.6931/17 C. -
Henry Primakoff Lecture: Neutrinoless Double-Beta Decay
Henry Primakoff Lecture: Neutrinoless Double-Beta Decay CENPA J.F. Wilkerson Center for Experimental Nuclear Physics and Astrophysics University of Washington April APS Meeting 2007 Renewed Impetus for 0νββ The recent discoveries of atmospheric, solar, and reactor neutrino oscillations and the corresponding realization that neutrinos are not massless particles, provides compelling arguments for performing neutrinoless double-beta decay (0νββ) experiments with increased sensitivity. 0νββ decay probes fundamental questions: • Tests one of nature's fundamental symmetries, Lepton number conservation. • The only practical technique able to determine if neutrinos might be their own anti-particles — Majorana particles. • If 0νββ is observed: • Provides a promising laboratory method for determining the overall absolute neutrino mass scale that is complementary to other measurement techniques. • Measurements in a series of different isotopes potentially can reveal the underlying interaction process(es). J.F. Wilkerson Primakoff Lecture: Neutrinoless Double-Beta Decay April APS Meeting 2007 Double-Beta Decay In a number of even-even nuclei, β-decay is energetically forbidden, while double-beta decay, from a nucleus of (A,Z) to (A,Z+2), is energetically allowed. A, Z-1 A, Z+1 0+ A, Z+3 A, Z ββ 0+ A, Z+2 J.F. Wilkerson Primakoff Lecture: Neutrinoless Double-Beta Decay April APS Meeting 2007 Double-Beta Decay In a number of even-even nuclei, β-decay is energetically forbidden, while double-beta decay, from a nucleus of (A,Z) to (A,Z+2), is energetically allowed. 2- 76As 0+ 76 Ge 0+ ββ 2+ Q=2039 keV 0+ 76Se 48Ca, 76Ge, 82Se, 96Zr 100Mo, 116Cd 128Te, 130Te, 136Xe, 150Nd J.F. -
Compilation and Evaluation of Fission Yield Nuclear Data Iaea, Vienna, 2000 Iaea-Tecdoc-1168 Issn 1011–4289
IAEA-TECDOC-1168 Compilation and evaluation of fission yield nuclear data Final report of a co-ordinated research project 1991–1996 December 2000 The originating Section of this publication in the IAEA was: Nuclear Data Section International Atomic Energy Agency Wagramer Strasse 5 P.O. Box 100 A-1400 Vienna, Austria COMPILATION AND EVALUATION OF FISSION YIELD NUCLEAR DATA IAEA, VIENNA, 2000 IAEA-TECDOC-1168 ISSN 1011–4289 © IAEA, 2000 Printed by the IAEA in Austria December 2000 FOREWORD Fission product yields are required at several stages of the nuclear fuel cycle and are therefore included in all large international data files for reactor calculations and related applications. Such files are maintained and disseminated by the Nuclear Data Section of the IAEA as a member of an international data centres network. Users of these data are from the fields of reactor design and operation, waste management and nuclear materials safeguards, all of which are essential parts of the IAEA programme. In the 1980s, the number of measured fission yields increased so drastically that the manpower available for evaluating them to meet specific user needs was insufficient. To cope with this task, it was concluded in several meetings on fission product nuclear data, some of them convened by the IAEA, that international co-operation was required, and an IAEA co-ordinated research project (CRP) was recommended. This recommendation was endorsed by the International Nuclear Data Committee, an advisory body for the nuclear data programme of the IAEA. As a consequence, the CRP on the Compilation and Evaluation of Fission Yield Nuclear Data was initiated in 1991, after its scope, objectives and tasks had been defined by a preparatory meeting. -
Electron Capture in Stars
Electron capture in stars K Langanke1;2, G Mart´ınez-Pinedo1;2;3 and R.G.T. Zegers4;5;6 1GSI Helmholtzzentrum f¨urSchwerionenforschung, D-64291 Darmstadt, Germany 2Institut f¨urKernphysik (Theoriezentrum), Department of Physics, Technische Universit¨atDarmstadt, D-64298 Darmstadt, Germany 3Helmholtz Forschungsakademie Hessen f¨urFAIR, GSI Helmholtzzentrum f¨ur Schwerionenforschung, D-64291 Darmstadt, Germany 4 National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA 5 Joint Institute for Nuclear Astrophysics: Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA 6 Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA E-mail: [email protected], [email protected], [email protected] Abstract. Electron captures on nuclei play an essential role for the dynamics of several astrophysical objects, including core-collapse and thermonuclear supernovae, the crust of accreting neutron stars in binary systems and the final core evolution of intermediate mass stars. In these astrophysical objects, the capture occurs at finite temperatures and at densities at which the electrons form a degenerate relativistic electron gas. The capture rates can be derived in perturbation theory where allowed nuclear transitions (Gamow-Teller transitions) dominate, except at the higher temperatures achieved in core-collapse supernovae where also forbidden transitions contribute significantly to the rates. There has been decisive progress in recent years in measuring Gamow-Teller (GT) strength distributions using novel experimental techniques based on charge-exchange reactions. These measurements provide not only data for the GT distributions of ground states for many relevant nuclei, but also serve as valuable constraints for nuclear models which are needed to derive the capture rates for the arXiv:2009.01750v1 [nucl-th] 3 Sep 2020 many nuclei, for which no data exist yet. -
Uranium Fact Sheet
Fact Sheet Adopted: December 2018 Health Physics Society Specialists in Radiation Safety 1 Uranium What is uranium? Uranium is a naturally occurring metallic element that has been present in the Earth’s crust since formation of the planet. Like many other minerals, uranium was deposited on land by volcanic action, dissolved by rainfall, and in some places, carried into underground formations. In some cases, geochemical conditions resulted in its concentration into “ore bodies.” Uranium is a common element in Earth’s crust (soil, rock) and in seawater and groundwater. Uranium has 92 protons in its nucleus. The isotope2 238U has 146 neutrons, for a total atomic weight of approximately 238, making it the highest atomic weight of any naturally occurring element. It is not the most dense of elements, but its density is almost twice that of lead. Uranium is radioactive and in nature has three primary isotopes with different numbers of neutrons. Natural uranium, 238U, constitutes over 99% of the total mass or weight, with 0.72% 235U, and a very small amount of 234U. An unstable nucleus that emits some form of radiation is defined as radioactive. The emitted radiation is called radioactivity, which in this case is ionizing radiation—meaning it can interact with other atoms to create charged atoms known as ions. Uranium emits alpha particles, which are ejected from the nucleus of the unstable uranium atom. When an atom emits radiation such as alpha or beta particles or photons such as x rays or gamma rays, the material is said to be undergoing radioactive decay (also called radioactive transformation). -
Proposed Method for Measuring the LET of Radiotherapeutic Particle Beams Stephen D
University of New Mexico UNM Digital Repository Physics & Astronomy ETDs Electronic Theses and Dissertations Fall 11-10-2017 Proposed Method for Measuring the LET of Radiotherapeutic Particle Beams Stephen D. Bello University of New Mexico - Main Campus Follow this and additional works at: https://digitalrepository.unm.edu/phyc_etds Part of the Astrophysics and Astronomy Commons, Health and Medical Physics Commons, Other Medical Sciences Commons, and the Other Physics Commons Recommended Citation Bello, Stephen D.. "Proposed Method for Measuring the LET of Radiotherapeutic Particle Beams." (2017). https://digitalrepository.unm.edu/phyc_etds/167 This Dissertation is brought to you for free and open access by the Electronic Theses and Dissertations at UNM Digital Repository. It has been accepted for inclusion in Physics & Astronomy ETDs by an authorized administrator of UNM Digital Repository. For more information, please contact [email protected]. Dedication To my father, who started my interest in physics, and my mother, who encouraged me to expand my mind. iii Acknowledgments I’d like to thank my advisor, Dr. Michael Holzscheiter, for his endless support, as well as putting up with my relentless grammatical errors concerning the focus of our research. And Dr. Shuang Luan for his feedback and criticism. iv Proposed Method for Measuring the LET of Radiotherapeutic Particle Beams by Stephen Donald Bello B.S., Physics & Astronomy, Ohio State University, 2012 M.S., Physics, University of New Mexico, 2017 Ph.D, Physics, University of New Mexico, 2017 Abstract The Bragg peak geometry of the depth dose distributions for hadrons allows for precise and e↵ective dose delivery to tumors while sparing neighboring healthy tis- sue. -
Physics Study Sheet for Math Pre-Test
AP Physics 1 Summer Assignments Dear AP Physics 1 Student, kudos to you for taking on the challenge of AP Physics! Attached you will find some physics-related math to work through before the first day of school. The problems require you to apply math concepts that were covered in algebra and trigonometry. Bring your completed sheets on the first day of school. Please familiarize yourself with the following websites. https://phet.colorado.edu/en/simulations/category/physics We will use this website extensively for physics simulations. These websites are good resources for physics concepts: http://hyperphysics.phy-astr.gsu.edu/hbase/hframe.html http://www.thephysicsaviary.com/APReview.html http://www.physicsclassroom.com/ http://www.learnapphysics.com/apphysics1and2/index.html https://openstax.org/subjects/science This website provides free online textbooks with links to online simulations. Finally, you will need a graph paper composition notebook on the first day of class. This serves as your Lab Notebook. I look forward to learning and teaching with you in the fall! Find time to relax and recharge over the summer. I will be checking my district email, so feel free to contact me with any questions and concerns. My email address is [email protected]. 1 Physics Study Sheet for Math Algebra Skills 1. Solve an equation for any variable. Solve the following for x. ay a) v + w = x2yz c) bx 2 1 1 21y b) d) x 32 x 32 2. Be able to reduce fractions containing powers of ten. 2 3 10 4 10 a) 10 b) 103 106 3.