Neutron Numbers 8, 20 and 28 Were Considered As Magic Over Several Decades
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KINETIC ANALYSIS of SUB-PROMPT-CRITICAL REACTOR ASSEMBLIES Hy S Das Theoretical Physics Division
BARC/1992/E/011 O 1 "o KINETIC ANALYSIS OF SUB-PROMPT-CRITICAL REACTOR ASSEMBLIES hy S Das Theoretical Physics Division 1992 BARC/1992/E/011 o UJ GOVERNMENT OF INDIA - AATOMIT C ENERGY COMMISSION U KINETIC ANALYSIS OF SUB-PROMPT-CRITICAL REACTOR ASSEMBLIES by S. Das Theoretical Physics Division BHABHA ATOMIC RESEARCH CENTRE BOMBAY, INDIA 1992 BARC/1992/E/011 BIBLIOBRAPHIC DESCRIPTION SHEET FOR TECHNICAL REPORT (as par IS i 94BNB - 1980) 01 Security classification i Unclassified 02 Distribution t External 03 Report status i New 04 Series i BARC External 05 Report type i Technical Report 06 Report No. i BARC/1992/E/011 07 Part No. or Volume No. i 08 Contract No. i 10 Title and subtitle i Kinetic analysis of sub-prompt- critical reactor assemblies 11 Collation i 14 p.f 4 figs., 1 tab. IS Project No. i 20 Personal author<s> i S. Das 21 Affiliation of author(s) i Theoretical Physics Division, Bhabha Atomic Research Centre, Bombay 22 Corporate author(s) i Bhabha Atomic Research Centre, Bombay - 400 085 23 Originating unit i Theoretical Physics Division, BARC, Bombay 24 Sponsor(s) Name i Department of Atomic Energy Type i Government 30 Date of submission i May 1992 31 Publication/Issue date i June 1992 Contd... (ii) 1 40 Publ i»h»r/Distributor t Head, Library and Information Division, Bhabha Atomic Rasaarch Contra, Bombay 42 Form of distribution t Hard Copy 50 Languaga of taxt i English 51 Languaga o-f summary i English 92 No. of references i % rafs. 53 Givas data on i 60 Abstract x Nautronic analysis of safaty-ralatad kinetics problams in experimental neutron multiplying assemblies has bean carried out using a sub-prompt-critical reactor model. -
PP and CNO-Cycle Nucleosynthesis: Kinetics and Numerical Modeling of Competitive Fusion Processes
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Supervised Undergraduate Student Research Chancellor’s Honors Program Projects and Creative Work 5-2012 PP and CNO-Cycle Nucleosynthesis: Kinetics and Numerical Modeling of Competitive Fusion Processes Matt Torrico [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_chanhonoproj Part of the Physical Processes Commons, and the Plasma and Beam Physics Commons Recommended Citation Torrico, Matt, "PP and CNO-Cycle Nucleosynthesis: Kinetics and Numerical Modeling of Competitive Fusion Processes" (2012). Chancellor’s Honors Program Projects. https://trace.tennessee.edu/utk_chanhonoproj/1557 This Dissertation/Thesis is brought to you for free and open access by the Supervised Undergraduate Student Research and Creative Work at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Chancellor’s Honors Program Projects by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. PP and CNO-Cycle Nucleosynthesis: Kinetics and Numerical Modeling of Competitive Fusion Processes M.N. TorricoA, M.W. GuidryA,B A Department of Physics and Astronomy, University of Tennessee, Knoxville, TN 37996, USA B Physics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA Signed on 21 April 2012 Abstract The very history of matter (and hence Man) is exquisitely coupled to the nuclear fusion processes that power the Sun and other stars. The fusion of hydrogen into helium and other thermonuclear fusion processes (collectively called nucleosynthesis processes) provides us with not only the energy to carry on our lives, but the very materials that constitute our very bodies and our world. -
Total Prompt Energy Release in the Neutron-Induced Fission Of
Nuclear Physics A 772 (2006) 113–137 Total prompt energy release in the neutron-induced fission of 235U, 238U, and 239Pu D.G. Madland Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA Received 12 January 2006; received in revised form 28 March 2006; accepted 29 March 2006 Available online 2 May 2006 Abstract This study addresses, for the first time, the total prompt energy release and its components for the fission of 235U, 238U, and 239Pu as a function of the kinetic energy of the neutron inducing the fission. The com- ponents are extracted from experimental measurements, where they exist, together with model-dependent calculation, interpolation, and extrapolation. While the components display clear dependencies upon the incident neutron energy, their sums display only weak, yet definite, energy dependencies. Also addressed is the total prompt energy deposition in fission for the same three systems. Results are presented in equation form. New measurements are recommended as a consequence of this study. © 2006 Elsevier B.V. All rights reserved. PACS: 24.75.+i; 25.85.Ec; 25.85.Ca; 27.90.+b Keywords: Energy release and energy deposition in neutron-induced fission; Experiment and Los Alamos model; 235U; 238U; 239Pu 1. Introduction This study is a consequence of open questions on the magnitudes of the total prompt energy re- lease in fission, the total prompt energy deposition in fission, the components of these quantities, and their dependencies upon the kinetic energy of the neutron inducing the fission. Our results are given in Eqs. (31)–(33) and Fig. 17 for the total prompt energy release in fission, and in Eqs. -
Lecture 7: "Basics of Star Formation and Stellar Nucleosynthesis" Outline
Lecture 7: "Basics of Star Formation and Stellar Nucleosynthesis" Outline 1. Formation of elements in stars 2. Injection of new elements into ISM 3. Phases of star-formation 4. Evolution of stars Mark Whittle University of Virginia Life Cycle of Matter in Milky Way Molecular clouds New clouds with gravitationally collapse heavier composition to form stellar clusters of stars are formed Molecular cloud Stars synthesize Most massive stars evolve He, C, Si, Fe via quickly and die as supernovae – nucleosynthesis heavier elements are injected in space Solar abundances • Observation of atomic absorption lines in the solar spectrum • For some (heavy) elements meteoritic data are used Solar abundance pattern: • Regularities reflect nuclear properties • Several different processes • Mixture of material from many, many stars 5 SolarNucleosynthesis abundances: key facts • Solar• Decreaseabundance in abundance pattern: with atomic number: - Large negative anomaly at Be, B, Li • Regularities reflect nuclear properties - Moderate positive anomaly around Fe • Several different processes 6 - Sawtooth pattern from odd-even effect • Mixture of material from many, many stars Origin of elements • The Big Bang: H, D, 3,4He, Li • All other nuclei were synthesized in stars • Stellar nucleosynthesis ⇔ 3 key processes: - Nuclear fusion: PP cycles, CNO bi-cycle, He burning, C burning, O burning, Si burning ⇒ till 40Ca - Photodisintegration rearrangement: Intense gamma-ray radiation drives nuclear rearrangement ⇒ 56Fe - Most nuclei heavier than 56Fe are due to neutron -
Radiation Detection from Fission
ORNL/TM-2004/234 RADIATION DETECTION FROM FISSION J. T. Mihalczo DOCUMENT AVAILABILITY Reports produced after January 1, 1996, are generally available free via the U.S. Department of Energy (DOE) Information Bridge. Web site http://www.osti.gov/bridge Reports produced before January 1, 1996, may be purchased by members of the public from the following source. National Technical Information Service 5285 Port Royal Road Springfield, VA 22161 Telephone 703-605-6000 (1-800-553-6847) TDD 703-487-4639 Fax 703-605-6900 E-mail [email protected] Web site http://www.ntis.gov/support/ordernowabout.htm Reports are available to DOE employees, DOE contractors, Energy Technology Data Exchange (ETDE) representatives, and International Nuclear Information System (INIS) representatives from the following source. Office of Scientific and Technical Information P.O. Box 62 Oak Ridge, TN 37831 Telephone 865-576-8401 Fax 865-576-5728 E-mail [email protected] Web site http://www.osti.gov/contact.html This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States government nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof. -
Nuclear Fission Dynamics: Past, Present, Needs, and Future
NT@UW-19-18,LA-UR-19-32211 Nuclear Fission Dynamics: Past, Present, Needs, and Future Aurel Bulgac,1 Shi Jin,1 and Ionel Stetcu2 1Department of Physics, University of Washington, Seattle, Washington 98195–1560, USA 2Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545, USA (Dated: March 23, 2020) Significant progress in the understanding of the fission process within a microscopic framework has been recently reported. Even though the complete description of this important nuclear reac- tion remains a computationally demanding task, recent developments in theoretical modeling and computational power have brought current microscopic simulations to the point where they can pro- vide guidance and constraints to phenomenological models, without making recourse to parameters. An accurate treatment compatible with our understanding of the inter-nucleon interactions should be able to describe the real-time dynamics of the fissioning system and could justify or rule out assumptions and approximations incompatible with the underlying universally accepted quantum- mechanical framework. Of particular importance are applications to observables that cannot be directly measured in experimental setups (such as the angular momentum distribution of the fission fragments, or the excitation energy sharing between the fission fragments, or fission of nuclei formed during the r-process), and their dependence of the excitation energy in the fissioning system. Even if accurate predictions are not within reach, being able to extract the trends with increasing exci- tation energy is important in various applications. The most advanced microscopic simulations of the fission process do not support the widely used assumption of adiabaticity of the large amplitude collective motion in fission, in particular for trajectories from the outer saddle towards the scission configuration. -
Pp-Chain and CNO Cycle
10 – pp-chain and CNO cycle introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 pp chain reaction in the Sun introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 2 10.1 - Hydrogen burning – ppI chain As a star forms from a giant cloud in the interstellar medium (protostar), density and temperature increase in its center. Fusion of hydrogen (1H) is the first long term nuclear energy source that can ignite. With only hydrogen available (for example, a first generation star) the ppI chain (see previous slide) is the only possible sequence of reactions. (other reaction chains require catalyst nuclei). The ppI chain proceeds as follows: 2 Step 1: p + p → He This does not work because 2He is unstable + (10.1) p + p → d + e + ve 3 (10.2) Step 2: d + p → He d d 4 He This does not work because the d abundance is + → too low. d + p leads to rapid destruction of d. 3 4 Step 3: He + p → Li Does not work because 4Li is unstable 3 He + d → 4 He + n Does not work because d abundance is too low 3 He + 3 He → 4 He + 2p (10.3) Last reaction is OK because Y3He gets large as there is no other rapid destruction. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 3 10.1.1 - S-factors for the pp chain All reactions in the pp-chain are charge-dependent. The cross section has the form given by Eq. (9.49) which can be cast in the form b − where 1 E σ ∝ e (10.4) A1A2 E b 31.28 Z Z A1/2 keV A = = 1 2 (10.5) A1 + A2 (10.6) Typical units for S(E) are keV barn. -
The History and Impact of the CNO Cycles in Nuclear Astrophysics
Phys. Perspect. 20 (2018) 124–158 Ó 2018 Springer International Publishing AG, part of Springer Nature 1422-6944/18/010124-35 https://doi.org/10.1007/s00016-018-0216-0 Physics in Perspective The History and Impact of the CNO Cycles in Nuclear Astrophysics Michael Wiescher* The carbon cycle, or Bethe-Weizsa¨cker cycle, plays an important role in astrophysics as one of the most important energy sources for quiescent and explosive hydrogen burning in stars. This paper presents the intellectual and historical background of the idea of the correlation between stellar energy production and the synthesis of the chemical elements in stars on the example of this cycle. In particular, it addresses the contributions of Carl Friedrich von Weizsa¨cker and Hans Bethe, who provided the first predictions of the carbon cycle. Further, the experimental verification of the predicted process as it developed over the following decades is discussed, as well as the extension of the initial carbon cycle to the carbon- nitrogen-oxygen (CNO) multi-cycles and the hot CNO cycles. This development emerged from the detailed experimental studies of the associated nuclear reactions over more than seven decades. Finally, the impact of the experimental and theoretical results on our present understanding of hydrogen burning in different stellar environments is presented, as well as the impact on our understanding of the chemical evolution of our universe. Key words: Carl Friedrich von Weizsa¨cker; Hans Bethe; Carbon cycle; CNO cycle. Introduction The energy source of the sun and all other stars became a topic of great interests in the physics community in the second half of the nineteenth century. -
Reactor Physics
REACTOR PHYSICS COURSE INTRODUCTION This Training Manual assumes prior knowledge of Nuclear Theory. It extends this information into a discussion of Reactor Physics, particularly as it relates to CANDU reactors. The course begins with the general principles of reactor configuration required to maintain a self- sustaining chain reaction. It continues with reactor dynamics (in both the critical and subcritical core), reactivity feedback effects (temperature effects, fission product poisoning, and fuel burnup), and ends with operational considerations (at low and high power). The material covers four main areas, subdivided into eight major sections as follows: • The Critical Reactor at Steady Power Output (Section 1) • The Dynamic Reactor (Sections 2 and 3) • Reactivity Feedback Effects (Sections 4, 5, and 6) • Reactor Operations (Sections 7 and 8) CNSC i Science and Reactor Fundamentals – Reactor Physics Technical Training Group TABLE OF CONTENTS Objectives 1 The Critical Reactor at Steady Power Output 9 1.0 INTRODUCTION 9 1.1 Fission 9 1.2 Harnessing Fission 15 1.3 Movement of Neutrons Through the CANDU lattice Lattice 18 1.4 The Finite Reactor 26 Response of The Critical Reactor to a Reactivity Change 31 2.0 INTRODUCTION 31 2.1 Exponential Power Rise 31 2.2 Corrections to Exponential Reactor Response 33 2.3 The Effect of Delayed Neutrons 36 2.4 Prompt Criticality 40 2.5 Power Rundown: The Prompt Drop 42 Responsiveness of The Subcritical Reactor 45 3.0 INTRODUCTION 45 3.1 Neutron Flux in a “Shut Down” Reactor 45 3.2 Dynamics in the Subcritical -
Stellar Nucleosynthesis
Stellar nucleosynthesis Stellar nucleosynthesis is the creation (nucleosynthesis) of chemical elements by nuclear fusion reactions within stars. Stellar nucleosynthesis has occurred since the original creation of hydrogen, helium and lithium during the Big Bang. As a predictive theory, it yields accurate estimates of the observed abundances of the elements. It explains why the observed abundances of elements change over time and why some elements and their isotopes are much more abundant than others. The theory was initially proposed by Fred Hoyle in 1946,[1] who later refined it in 1954.[2] Further advances were made, especially to nucleosynthesis by neutron capture of the elements heavier than iron, by Margaret Burbidge, Geoffrey Burbidge, William Alfred Fowler and Hoyle in their famous 1957 B2FH paper,[3] which became one of the most heavily cited papers in astrophysics history. Stars evolve because of changes in their composition (the abundance of their constituent elements) over their lifespans, first by burning hydrogen (main sequence star), then helium (red giant star), and progressively burning higher elements. However, this does not by itself significantly alter the abundances of elements in the universe as the elements are contained within the star. Later in its life, a low-mass star will slowly eject its atmosphere via stellar wind, forming a planetary nebula, while a higher–mass star will eject mass via a sudden catastrophic event called a supernova. The term supernova nucleosynthesis is used to describe the creation of elements during the explosion of a massive star or white dwarf. The advanced sequence of burning fuels is driven by gravitational collapse and its associated heating, resulting in the subsequent burning of carbon, oxygen and silicon. -
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1- TOPIC: 292001 KNOWLEDGE: K1.02 [3.0/3.1] QID: B45 the Term “Neutron Generation Time” Is Defined As the Average Time Betw
NRC Generic Fundamentals Examination Question Bank--BWR May 2020 TOPIC: 292001 KNOWLEDGE: K1.02 [3.0/3.1] QID: B45 The term “neutron generation time” is defined as the average time between... A. neutron absorption and the resulting fission. B. the production of a delayed neutron and subsequent neutron thermalization. C. neutron absorption producing a fission and absorption or leakage of resultant neutrons. D. neutron thermalization and subsequent neutron absorption. ANSWER: C. TOPIC: 292001 KNOWLEDGE: K1.02 [3.0/3.1] QID: B174 Which one of the following is the definition of the term, prompt neutron? A. A high-energy neutron emitted from a neutron precursor, immediately after the fission process. B. A neutron with an energy level greater than 0.1 MeV, emitted in less than 1.0 x 10-4 seconds following a nuclear fission. C. A neutron emitted in less than 1.0 x 10-14 seconds following a nuclear fission. D. A neutron emitted as a result of a gamma-neutron or alpha-neutron reaction. ANSWER: C. -1- Neutrons NRC Generic Fundamentals Examination Question Bank--BWR May 2020 TOPIC: 292001 KNOWLEDGE: K1.02 [3.0/3.1] QID: B245 Delayed neutrons are neutrons that... A. have reached thermal equilibrium with the surrounding medium. B. are expelled within 1.0 x 10-14 seconds of the fission event. C. are expelled with the lowest average kinetic energy of all fission neutrons. D. are responsible for the majority of U-235 fissions. ANSWER: C. TOPIC: 292001 KNOWLEDGE: K1.02 [3.0/3.1] QID: B1146 (P1945) Which one of the following types of neutrons has an average neutron generation lifetime of 12.5 seconds? A. -
Module 2: Reactor Theory (Neutron Characteristics)
DOE Fundamentals NUCLEAR PHYSICS AND REACTOR THEORY Module 2: Reactor Theory (Neutron Characteristics) NUCLEAR PHYSICS AND REACTOR THEORY TABLE OF CONTENTS Table of Co nte nts TABLE OF CONTENTS ................................................................................................... i LIST OF FIGURES .......................................................................................................... iii LIST OF TABLES ............................................................................................................iv REFERENCES ................................................................................................................ v OBJECTIVES ..................................................................................................................vi NEUTRON SOURCES .................................................................................................... 1 Neutron Sources .......................................................................................................... 1 Intrinsic Neutron Sources ............................................................................................. 1 Installed Neutron Sources ............................................................................................ 3 Summary...................................................................................................................... 4 NUCLEAR CROSS SECTIONS AND NEUTRON FLUX ................................................. 5 Introduction .................................................................................................................