CHAPTER 2 the Nucleus and Radioactive Decay
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The R-Process Nucleosynthesis and Related Challenges
EPJ Web of Conferences 165, 01025 (2017) DOI: 10.1051/epjconf/201716501025 NPA8 2017 The r-process nucleosynthesis and related challenges Stephane Goriely1,, Andreas Bauswein2, Hans-Thomas Janka3, Oliver Just4, and Else Pllumbi3 1Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, 1050 Brussels, Belgium 2Heidelberger Institut fr¨ Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany 3Max-Planck-Institut für Astrophysik, Postfach 1317, 85741 Garching, Germany 4Astrophysical Big Bang Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama, 351-0198, Japan Abstract. The rapid neutron-capture process, or r-process, is known to be of fundamental importance for explaining the origin of approximately half of the A > 60 stable nuclei observed in nature. Recently, special attention has been paid to neutron star (NS) mergers following the confirmation by hydrodynamic simulations that a non-negligible amount of matter can be ejected and by nucleosynthesis calculations combined with the predicted astrophysical event rate that such a site can account for the majority of r-material in our Galaxy. We show here that the combined contribution of both the dynamical (prompt) ejecta expelled during binary NS or NS-black hole (BH) mergers and the neutrino and viscously driven outflows generated during the post-merger remnant evolution of relic BH-torus systems can lead to the production of r-process elements from mass number A > 90 up to actinides. The corresponding abundance distribution is found to reproduce the∼ solar distribution extremely well. It can also account for the elemental distributions observed in low-metallicity stars. However, major uncertainties still affect our under- standing of the composition of the ejected matter. -
Photofission Cross Sections of 238U and 235U from 5.0 Mev to 8.0 Mev Robert Andrew Anderl Iowa State University
Iowa State University Capstones, Theses and Retrospective Theses and Dissertations Dissertations 1972 Photofission cross sections of 238U and 235U from 5.0 MeV to 8.0 MeV Robert Andrew Anderl Iowa State University Follow this and additional works at: https://lib.dr.iastate.edu/rtd Part of the Nuclear Commons, and the Oil, Gas, and Energy Commons Recommended Citation Anderl, Robert Andrew, "Photofission cross sections of 238U and 235U from 5.0 MeV to 8.0 MeV " (1972). Retrospective Theses and Dissertations. 4715. https://lib.dr.iastate.edu/rtd/4715 This Dissertation is brought to you for free and open access by the Iowa State University Capstones, Theses and Dissertations at Iowa State University Digital Repository. It has been accepted for inclusion in Retrospective Theses and Dissertations by an authorized administrator of Iowa State University Digital Repository. For more information, please contact [email protected]. INFORMATION TO USERS This dissertation was produced from a microfilm copy of the original document. While the most advanced technological means to photograph and reproduce this document have been used, the quality is heavily dependent upon the quality of the original submitted. The following explanation of techniques is provided to help you understand markings or patterns which may appear on this reproduction, 1. The sign or "target" for pages apparently lacking from the document photographed is "Missing Page(s)". If it was possible to obtain the missing page(s) or section, they are spliced into the film along with adjacent pages. This may have necessitated cutting thru an image and duplicating adjacent pages to insure you complete continuity, 2. -
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. -
1 Lecture Notes in Nuclear Structure Physics B. Alex Brown November
1 Lecture Notes in Nuclear Structure Physics B. Alex Brown November 2005 National Superconducting Cyclotron Laboratory and Department of Physics and Astronomy Michigan State University, E. Lansing, MI 48824 CONTENTS 2 Contents 1 Nuclear masses 6 1.1 Masses and binding energies . 6 1.2 Q valuesandseparationenergies . 10 1.3 Theliquid-dropmodel .......................... 18 2 Rms charge radii 25 3 Charge densities and form factors 31 4 Overview of nuclear decays 40 4.1 Decaywidthsandlifetimes. 41 4.2 Alphaandclusterdecay ......................... 42 4.3 Betadecay................................. 51 4.3.1 BetadecayQvalues ....................... 52 4.3.2 Allowedbetadecay ........................ 53 4.3.3 Phase-space for allowed beta decay . 57 4.3.4 Weak-interaction coupling constants . 59 4.3.5 Doublebetadecay ........................ 59 4.4 Gammadecay............................... 61 4.4.1 Reduced transition probabilities for gamma decay . .... 62 4.4.2 Weisskopf units for gamma decay . 65 5 The Fermi gas model 68 6 Overview of the nuclear shell model 71 7 The one-body potential 77 7.1 Generalproperties ............................ 77 7.2 Theharmonic-oscillatorpotential . ... 79 7.3 Separation of intrinsic and center-of-mass motion . ....... 81 7.3.1 Thekineticenergy ........................ 81 7.3.2 Theharmonic-oscillator . 83 8 The Woods-Saxon potential 87 8.1 Generalform ............................... 87 8.2 Computer program for the Woods-Saxon potential . .... 91 8.2.1 Exampleforboundstates . 92 8.2.2 Changingthepotentialparameters . 93 8.2.3 Widthofanunboundstateresonance . 94 8.2.4 Width of an unbound state resonance at a fixed energy . 95 9 The general many-body problem for fermions 97 CONTENTS 3 10 Conserved quantum numbers 101 10.1 Angularmomentum. 101 10.2Parity .................................. -
Radioactive Decay
North Berwick High School Department of Physics Higher Physics Unit 2 Particles and Waves Section 3 Fission and Fusion Section 3 Fission and Fusion Note Making Make a dictionary with the meanings of any new words. Einstein and nuclear energy 1. Write down Einstein’s famous equation along with units. 2. Explain the importance of this equation and its relevance to nuclear power. A basic model of the atom 1. Copy the components of the atom diagram and state the meanings of A and Z. 2. Copy the table on page 5 and state the difference between elements and isotopes. Radioactive decay 1. Explain what is meant by radioactive decay and copy the summary table for the three types of nuclear radiation. 2. Describe an alpha particle, including the reason for its short range and copy the panel showing Plutonium decay. 3. Describe a beta particle, including its range and copy the panel showing Tritium decay. 4. Describe a gamma ray, including its range. Fission: spontaneous decay and nuclear bombardment 1. Describe the differences between the two methods of decay and copy the equation on page 10. Nuclear fission and E = mc2 1. Explain what is meant by the terms ‘mass difference’ and ‘chain reaction’. 2. Copy the example showing the energy released during a fission reaction. 3. Briefly describe controlled fission in a nuclear reactor. Nuclear fusion: energy of the future? 1. Explain why nuclear fusion might be a preferred source of energy in the future. 2. Describe some of the difficulties associated with maintaining a controlled fusion reaction. -
Arxiv:1901.01410V3 [Astro-Ph.HE] 1 Feb 2021 Mental Information Is Available, and One Has to Rely Strongly on Theoretical Predictions for Nuclear Properties
Origin of the heaviest elements: The rapid neutron-capture process John J. Cowan∗ HLD Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA Christopher Snedeny Department of Astronomy, University of Texas, 2515 Speedway, Austin, TX 78712-1205, USA James E. Lawlerz Physics Department, University of Wisconsin-Madison, 1150 University Avenue, Madison, WI 53706-1390, USA Ani Aprahamianx and Michael Wiescher{ Department of Physics and Joint Institute for Nuclear Astrophysics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA Karlheinz Langanke∗∗ GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany and Institut f¨urKernphysik (Theoriezentrum), Fachbereich Physik, Technische Universit¨atDarmstadt, Schlossgartenstraße 2, 64298 Darmstadt, Germany Gabriel Mart´ınez-Pinedoyy GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany; Institut f¨urKernphysik (Theoriezentrum), Fachbereich Physik, Technische Universit¨atDarmstadt, Schlossgartenstraße 2, 64298 Darmstadt, Germany; and Helmholtz Forschungsakademie Hessen f¨urFAIR, GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany Friedrich-Karl Thielemannzz Department of Physics, University of Basel, Klingelbergstrasse 82, 4056 Basel, Switzerland and GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany (Dated: February 2, 2021) The production of about half of the heavy elements found in nature is assigned to a spe- cific astrophysical nucleosynthesis process: the rapid neutron capture process (r-process). Although this idea has been postulated more than six decades ago, the full understand- ing faces two types of uncertainties/open questions: (a) The nucleosynthesis path in the nuclear chart runs close to the neutron-drip line, where presently only limited experi- arXiv:1901.01410v3 [astro-ph.HE] 1 Feb 2021 mental information is available, and one has to rely strongly on theoretical predictions for nuclear properties. -
Two-Proton Radioactivity 2
Two-proton radioactivity Bertram Blank ‡ and Marek P loszajczak † ‡ Centre d’Etudes Nucl´eaires de Bordeaux-Gradignan - Universit´eBordeaux I - CNRS/IN2P3, Chemin du Solarium, B.P. 120, 33175 Gradignan Cedex, France † Grand Acc´el´erateur National d’Ions Lourds (GANIL), CEA/DSM-CNRS/IN2P3, BP 55027, 14076 Caen Cedex 05, France Abstract. In the first part of this review, experimental results which lead to the discovery of two-proton radioactivity are examined. Beyond two-proton emission from nuclear ground states, we also discuss experimental studies of two-proton emission from excited states populated either by nuclear β decay or by inelastic reactions. In the second part, we review the modern theory of two-proton radioactivity. An outlook to future experimental studies and theoretical developments will conclude this review. PACS numbers: 23.50.+z, 21.10.Tg, 21.60.-n, 24.10.-i Submitted to: Rep. Prog. Phys. Version: 17 December 2013 arXiv:0709.3797v2 [nucl-ex] 23 Apr 2008 Two-proton radioactivity 2 1. Introduction Atomic nuclei are made of two distinct particles, the protons and the neutrons. These nucleons constitute more than 99.95% of the mass of an atom. In order to form a stable atomic nucleus, a subtle equilibrium between the number of protons and neutrons has to be respected. This condition is fulfilled for 259 different combinations of protons and neutrons. These nuclei can be found on Earth. In addition, 26 nuclei form a quasi stable configuration, i.e. they decay with a half-life comparable or longer than the age of the Earth and are therefore still present on Earth. -
2.3 Neutrino-Less Double Electron Capture - Potential Tool to Determine the Majorana Neutrino Mass by Z.Sujkowski, S Wycech
DEPARTMENT OF NUCLEAR SPECTROSCOPY AND TECHNIQUE 39 The above conservatively large systematic hypothesis. TIle quoted uncertainties will be soon uncertainty reflects the fact that we did not finish reduced as our analysis progresses. evaluating the corrections fully in the current analysis We are simultaneously recording a large set of at the time of this writing, a situation that will soon radiative decay events for the processes t e'v y change. This result is to be compared with 1he and pi-+eN v y. The former will be used to extract previous most accurate measurement of McFarlane the ratio FA/Fv of the axial and vector form factors, a et al. (Phys. Rev. D 1984): quantity of great and longstanding interest to low BR = (1.026 ± 0.039)'1 I 0 energy effective QCD theory. Both processes are as well as with the Standard Model (SM) furthermore very sensitive to non- (V-A) admixtures in prediction (Particle Data Group - PDG 2000): the electroweak lagLangian, and thus can reveal BR = (I 038 - 1.041 )*1 0-s (90%C.L.) information on physics beyond the SM. We are currently analyzing these data and expect results soon. (1.005 - 1.008)* 1W') - excl. rad. corr. Tale 1 We see that even working result strongly confirms Current P1IBETA event sxpelilnentstatistics, compared with the the validity of the radiative corrections. Another world data set. interesting comparison is with the prediction based on Decay PIBETA World data set the most accurate evaluation of the CKM matrix n >60k 1.77k element V d based on the CVC hypothesis and ihce >60 1.77_ _ _ results -
14. Structure of Nuclei Particle and Nuclear Physics
14. Structure of Nuclei Particle and Nuclear Physics Dr. Tina Potter Dr. Tina Potter 14. Structure of Nuclei 1 In this section... Magic Numbers The Nuclear Shell Model Excited States Dr. Tina Potter 14. Structure of Nuclei 2 Magic Numbers Magic Numbers = 2; 8; 20; 28; 50; 82; 126... Nuclei with a magic number of Z and/or N are particularly stable, e.g. Binding energy per nucleon is large for magic numbers Doubly magic nuclei are especially stable. Dr. Tina Potter 14. Structure of Nuclei 3 Magic Numbers Other notable behaviour includes Greater abundance of isotopes and isotones for magic numbers e.g. Z = 20 has6 stable isotopes (average=2) Z = 50 has 10 stable isotopes (average=4) Odd A nuclei have small quadrupole moments when magic First excited states for magic nuclei higher than neighbours Large energy release in α, β decay when the daughter nucleus is magic Spontaneous neutron emitters have N = magic + 1 Nuclear radius shows only small change with Z, N at magic numbers. etc... etc... Dr. Tina Potter 14. Structure of Nuclei 4 Magic Numbers Analogy with atomic behaviour as electron shells fill. Atomic case - reminder Electrons move independently in central potential V (r) ∼ 1=r (Coulomb field of nucleus). Shells filled progressively according to Pauli exclusion principle. Chemical properties of an atom defined by valence (unpaired) electrons. Energy levels can be obtained (to first order) by solving Schr¨odinger equation for central potential. 1 E = n = principle quantum number n n2 Shell closure gives noble gas atoms. Are magic nuclei analogous to the noble gas atoms? Dr. -
Mass Defect & Binding Energy
Sem-3 CC7 Nuclear Physics Mass Defect & Binding Energy According to nuclear particle experiments, the total mass of a nucleus (mnuc) is less than the sum of the masses of its constituent nucleons (protons and neutrons). For a nucleus with Z protons and mass number A, the mass difference or mass defect is given by Δm= Zmp + (A−Z)mn − mnuc where Zmp is the total mass of the protons, (A−Z)mn is the total mass of the neutrons, and mnuc is the mass of the nucleus. According to Einstein’s special theory of relativity, mass is a measure of the total energy of a system (E=mc2). The energy equivalent to mass defect is alled the binding energy B of the nucleus. Thus 2 B= [Zmp + (A−Z)mn − mnuc] c The binding energy is equal to the amount of energy released in forming the nucleus. Example 1. Calculate the mass defect and the binding energy of the deuteron. The mass of the −27 deuteron is mD=3.34359×10 kg or 2.014102u. Solution For the deuteron Z=1 and A=2. The mass defect for the deuteron is Δm=mp+mn−mD=1.008665 u+ 1.007825 u- 2.014102u = 0.002388u The binding energy of the deuteron is then B= Δm c2= Δm ×931.5 MeV/u=2.224MeV. Over two million electron volts are needed to break apart a deuteron into a proton and a neutron. This very large value indicates the great strength of the nuclear force. By comparison, the greatest amount of energy required to liberate an electron bound to a hydrogen atom by an attractive Coulomb force (an electromagnetic force) is about 10 eV. -
Problem Set 3 Solutions
22.01 Fall 2016, Problem Set 3 Solutions October 9, 2016 Complete all the assigned problems, and do make sure to show your intermediate work. 1 Activity and Half Lives 1. Given the half lives and modern-day abundances of the three natural isotopes of uranium, calculate the isotopic fractions of uranium when the Earth first formed 4.5 billion years ago. Today, uranium consists of 0.72% 235U, 99.2745% 238U, and 0.0055% 234U. However, it is clear that the half life of 234U (245,500 years) is so short compared to the lifetime of the Earth (4,500,000,000 years) that it would have all decayed away had there been some during the birth of the Earth. Therefore, we look a little closer, and find that 234U is an indirect decay product of 238U, by tracing it back from its parent nuclides on the KAERI table: α β− β− 238U −! 234T h −! 234P a −! 234U (1) Therefore we won’t consider there being any more 234U than would normally be in equi librium with the 238U around at the time. We set up the two remaining equations as follows: −t t ;235 −t t ;238 = 1=2 = 1=2 N235 = N0235 e N238 = N0238 e (2) Using the current isotopic abundances from above as N235 and N238 , the half lives from n 9 t 1 1 the KAERI Table of Nuclides t =2;235 = 703800000 y; t =2;238 = 4:468 · 10 y , and the lifetime of the earth in years (keeping everything in the same units), we arrive at the following expressions for N0235 and N0238 : N235 0:0072 N238 0:992745 N0235 =−t = 9 = 4:307N0238 =−t = 9 = 2:718 (3) =t1 ;235 −4:5·10 =7:038·108 =t1 ;238 −4:5·10 =4:468·109 e =2 e e =2 e Finally, taking the ratios of these two relative abundances gives us absolute abundances: 4:307 2:718 f235 = = 0:613 f238 = = 0:387 (4) 4:307 + 2:718 4:307 + 2:718 235U was 61.3% abundant, and 238U was 38.7% abundant. -
Iron-57 of Its Isotopes and Has an Sum of Protons + Neutrons 26 Fe Average Mass As Determined by a in the Nucleus
Elements - elements are pure homogeneous forms of matter Solid Liquid Gas Plamsa •constant volume & shape •constant volume but takes •varaible shape and volume •like a gas except it •very low compressibility on the shape of container that fills the container is composed of ions; •particles vibrate in place •low compressibility •high compressibility an ion is charged •highly ordered arrangement •random particle movement •complete freedom of motion atom or group of •do not flow or diffuse •moderate disorder •extreme disorder atoms. •strongest attractive forces •can flow and diffuse •flow and diffuse easily •examples: between particles •weaker attractive forces •weakest attractive forces - flames •generally more dense than •more dense than gases •least dense state - atmosphere of stars liquids •exert a pressure easily - a comet's tail Matter NO YES Pure Substance Can it be separated Mixture by physical means? Can it be decomposed by Is the mixture composition ordinary chemical means? identical throughout; uniform? NO YES YES NO element compound homogeneous heterogenous mixture mixture Co,Fe,S,H,O,C FeS, H2O, H2SO4 steel, air, blood, steam, wet iron, solution of sulfuric acid Cannot be separated Can be decomposed and rust on steel chemcially into simple chemcially separated Uniform appearance, Appearance, composition, substances into simple substances. composition and and properties are variable properties throughout in different parts of the sample Isotopes Is a mass number attached to the element? NO YES All atoms of the same element are not exactly alike mass number attached mass number equals the 57 The element is as a mixture also can be written as iron-57 of its isotopes and has an sum of protons + neutrons 26 Fe average mass as determined by a in the nucleus.