Direct Measurement of the Neutron
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Neutron Interactions and Dosimetry Outline Introduction Tissue
Outline • Neutron dosimetry Neutron Interactions and – Thermal neutrons Dosimetry – Intermediate-energy neutrons – Fast neutrons Chapter 16 • Sources of neutrons • Mixed field dosimetry, paired dosimeters F.A. Attix, Introduction to Radiological • Rem meters Physics and Radiation Dosimetry Introduction Tissue composition • Consider neutron interactions with the majority tissue elements H, O, C, and N, and the resulting absorbed dose • Because of the short ranges of the secondary charged particles that are produced in such interactions, CPE is usually well approximated • Since no bremsstrahlung x-rays are generated, the • The ICRU composition for muscle has been assumed in absorbed dose can be assumed to be equal to the most cases for neutron-dose calculations, lumping the kerma at any point in neutron fields at least up to 1.1% of “other” minor elements together with oxygen to an energy E ~ 20 MeV make a simple four-element (H, O, C, N) composition Neutron kinetic energy Neutron kinetic energy • Neutron fields are divided into three • Thermal neutrons, by definition, have the most probable categories based on their kinetic energy: kinetic energy E=kT=0.025eV at T=20C – Thermal (E<0.5 eV) • Neutrons up to 0.5eV are considered “thermal” due to simplicity of experimental test after they emerge from – Intermediate-energy (0.5 eV<E<10 keV) moderator material – Fast (E>10 keV) • Cadmium ratio test: • Differ by their primary interactions in tissue – Gold foil can be activated through 197Au(n,)198Au interaction and resulting biological effects -
Concrete Analysis by Neutron-Capture Gamma Rays Using Californium 252
CONCRETE ANALYSIS BY NEUTRON-CAPTURE GAMMA RAYS USING CALIFORNIUM 252 Dick Duffey, College of Engineering, University of Maryland; Peter F. Wiggins, Naval Systems Engineering Department, U.S. Naval Academy; Frank E. Senftle, U.S. Geological Survey; and A. A. El Kady, United Arab Republic Atomic Energy Establishment, Cairo The feasibility of analyzing concrete and cement by a measurement of the neutron-capture or prompt gamma rays was investigated; a 100-ug californium-252 source was used to supply the neutrons. A lithium drifted germanium crystal detected the capture gamma rays emitted. The capture gamma rays from cement, sand, and 3 coarse aggregates-quartzite gravel, limestone, and diabase--:were studied. Concrete blocks made from these materials were then tested. The capture gamma ray response of the calcium, silicon, and iron in the concrete blocks was in accord with the elements identified in the mix materials. The principal spectral lines used were the 6.42 MeV line of calcium, the 4.93 MeV line of silicon, and the doublet of iron at about 7 .64 MeV. The aluminum line at 7. 72 MeV was ob served in some cases but at a lower intensity with the limited electronic equipment available. This nuclear spectroscopic technique offers a possi ble method of determining the components of sizable concrete samples in a nondestructive, in situ manner. In addition, the neutron-capture gamma ray technique might find application in control of the concrete and cement processes and furnish needed information on production operations and inventories. • FROM THE point of view of the geochemical analyst, concrete may be considered as rock relocated and reformed at the convenience of the engineer. -
Cosmogenic Production As a Background in Searching For
Cosmogenic Production as a Background in Searching for Rare Physics Processes D.-M. Mei a , Z.-B. Yin a,b,c,1, S. R. Elliott d aDepartment of Physics, The University of South Dakota, Vermillion, South Dakota 57069 bInstitute of Particle Physics, Huazhong Normal University, Wuhan 430079, China cKey Laboratory of Quark & Lepton Physics (Huazhong Normal University), Ministry of Education, China dLos Alamos National Laboratory, Los Alamos, New Mexico 87545 Abstract We revisit calculations of the cosmogenic production rates for several long-lived iso- topes that are potential sources of background in searching for rare physics processes such as the detection of dark matter and neutrinoless double-beta decay. Using up- dated cosmic-ray neutron flux measurements, we use TALYS 1.0 to investigate the cosmogenic activation of stable isotopes of several detector targets and find that the cosmogenic isotopes produced inside the target materials and cryostat can result in large backgrounds for dark matter searches and neutrinoless double-beta decay. We use previously published low-background HPGe data to constrain the production of 3H on the surface and the upper limit is consistent with our calculation. We note that cosmogenic production of several isotopes in various targets can generate po- arXiv:0903.2273v1 [nucl-ex] 12 Mar 2009 tential backgrounds for dark matter detection and neutrinoless double-beta decay with a massive detector, thus great care should be taken to limit and/or deal with the cosmogenic activation of the targets. Key words: Cosmogenic activation, Dark matter detection, Double-beta decay PACS: 13.85.Tp, 23.40-s, 25.40.Sc, 28.41.Qb, 95.35.+d, 29.40.Wk Email address: [email protected] (D.-M. -
Nucleosynthesis
Nucleosynthesis Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons. The first nuclei were formed about three minutes after the Big Bang, through the process called Big Bang nucleosynthesis. Seventeen minutes later the universe had cooled to a point at which these processes ended, so only the fastest and simplest reactions occurred, leaving our universe containing about 75% hydrogen, 24% helium, and traces of other elements such aslithium and the hydrogen isotope deuterium. The universe still has approximately the same composition today. Heavier nuclei were created from these, by several processes. Stars formed, and began to fuse light elements to heavier ones in their cores, giving off energy in the process, known as stellar nucleosynthesis. Fusion processes create many of the lighter elements up to and including iron and nickel, and these elements are ejected into space (the interstellar medium) when smaller stars shed their outer envelopes and become smaller stars known as white dwarfs. The remains of their ejected mass form theplanetary nebulae observable throughout our galaxy. Supernova nucleosynthesis within exploding stars by fusing carbon and oxygen is responsible for the abundances of elements between magnesium (atomic number 12) and nickel (atomic number 28).[1] Supernova nucleosynthesis is also thought to be responsible for the creation of rarer elements heavier than iron and nickel, in the last few seconds of a type II supernova event. The synthesis of these heavier elements absorbs energy (endothermic process) as they are created, from the energy produced during the supernova explosion. Some of those elements are created from the absorption of multiple neutrons (the r-process) in the period of a few seconds during the explosion. -
1663-29-Othernuclearreaction.Pdf
it’s not fission or fusion. It’s not alpha, beta, or gamma dosimeter around his neck to track his exposure to radiation decay, nor any other nuclear reaction normally discussed in in the lab. And when he’s not in the lab, he can keep tabs on his an introductory physics textbook. Yet it is responsible for various experiments simultaneously from his office computer the existence of more than two thirds of the elements on the with not one or two but five widescreen monitors—displaying periodic table and is virtually ubiquitous anywhere nuclear graphs and computer codes without a single pixel of unused reactions are taking place—in nuclear reactors, nuclear bombs, space. Data printouts pinned to the wall on the left side of the stellar cores, and supernova explosions. office and techno-scribble densely covering the whiteboard It’s neutron capture, in which a neutron merges with an on the right side testify to a man on a mission: developing, or atomic nucleus. And at first blush, it may even sound deserving at least contributing to, a detailed understanding of complex of its relative obscurity, since neutrons are electrically neutral. atomic nuclei. For that, he’ll need to collect and tabulate a lot For example, add a neutron to carbon’s most common isotope, of cold, hard data. carbon-12, and you just get carbon-13. It’s slightly heavier than Mosby’s primary experimental apparatus for doing this carbon-12, but in terms of how it looks and behaves, the two is the Detector for Advanced Neutron Capture Experiments are essentially identical. -
Primordial Nucleosynthesis: from Precision Cosmology To
DSF-20/2008, FERMILAB-PUB-08-216-A, IFIC/08-37 Primordial Nucleosynthesis: from precision cosmology to fundamental physics Fabio Iocco a1 , Gianpiero Mangano b, Gennaro Miele b,c, Ofelia Pisanti b, Pasquale D. Serpico d2 aINAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy bDip. Scienze Fisiche, Universit`adi Napoli Federico II & INFN, Sez. di Napoli, Complesso Univ. Monte S. Angelo, Via Cintia, I-80126 Napoli, Italy c Instituto de F´ısica Corpuscular (CSIC-Universitat de Val`encia), Ed. Institutos de Investigaci´on, Apartado de Correos 22085, E-46071 Val`encia, Spain dCenter for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510-0500, USA Abstract We present an up-to-date review of Big Bang Nucleosynthesis (BBN). We discuss the main improvements which have been achieved in the past two decades on the overall theoretical framework, summarize the impact of new experimental results on nuclear reaction rates, and critically re-examine the astrophysical determinations of light nuclei abundances. We report then on how BBN can be used as a powerful test of new physics, constraining a wide range of ideas and theoretical models of fundamental interactions beyond the standard model of strong and electroweak forces and Einstein’s general relativity. Key words: Primordial Nucleosynthesis; Early Universe; Physics Beyond the arXiv:0809.0631v2 [astro-ph] 16 Apr 2009 Standard Model PACS: 98.80.Ft; 26.35.+c; 98.62.Ai Contents 1 Introduction 3 2 Standard Cosmology 6 1 Present address: Institut -
Oxidation-Reduction Alternating Copolymerization of Germylene and N-Phenyl-P-Quinoneimine
Polymer Journal (2015) 47, 31–36 & 2015 The Society of Polymer Science, Japan (SPSJ) All rights reserved 0032-3896/15 www.nature.com/pj ORIGINAL ARTICLE Oxidation-reduction alternating copolymerization of germylene and N-phenyl-p-quinoneimine Satoru Iwata1, Mitsunori Abe1, Shin-ichiro Shoda1 and Shiro Kobayashi1,2 The germylenes bis[bis(trimethylsilyl)amido]germanium (1a) and bis[t-butyl-trimethylsilyl]amido]germanium (1b) were reacted with N-phenyl-p-quinoneimine (2) to give copolymers (3a and 3b) with alternating tetravalent germanium and p-aminophenol units. The copolymerization took place smoothly at 0 °C without added catalyst or initiator. 1 acted as a reductant monomer, and 2 acted as an oxidant monomer (oxidation-reduction alternating copolymerization). Product copolymers were obtained in very high yields and had high molecular weights. The copolymers were soluble in toluene, benzene, n-hexane and chloroform, whereas they were insoluble in acetonitrile and acetone. Additionally, they were stable toward hydrolytic degradation. Electron spin resonance (ESR) spectroscopic studies of the reaction suggested a structure of a stable germyl radical and a plausible mechanism of biradical copolymerization. Polymer Journal (2015) 47, 31–36; doi:10.1038/pj.2014.84; published online 8 October 2014 INTRODUCTION investigations.10 Five- and six-membered cyclic germylenes, conver- Divalent germanium compounds (germylenes) and their tin analogs sely, were copolymerized with p-benzoquinone derivatives in similar (stannylenes) continue to attract -
STUDY of the NEUTRON and PROTON CAPTURE REACTIONS 10,11B(N, ), 11B(P, ), 14C(P, ), and 15N(P, ) at THERMAL and ASTROPHYSICAL ENERGIES
STUDY OF THE NEUTRON AND PROTON CAPTURE REACTIONS 10,11B(n, ), 11B(p, ), 14C(p, ), AND 15N(p, ) AT THERMAL AND ASTROPHYSICAL ENERGIES SERGEY DUBOVICHENKO*,†, ALBERT DZHAZAIROV-KAKHRAMANOV*,† *V. G. Fessenkov Astrophysical Institute “NCSRT” NSA RK, 050020, Observatory 23, Kamenskoe plato, Almaty, Kazakhstan †Institute of Nuclear Physics CAE MINT RK, 050032, str. Ibragimova 1, Almaty, Kazakhstan *[email protected] †[email protected] We have studied the neutron-capture reactions 10,11B(n, ) and the role of the 11B(n, ) reaction in seeding r-process nucleosynthesis. The possibility of the description of the available experimental data for cross sections of the neutron capture reaction on 10B at thermal and astrophysical energies, taking into account the resonance at 475 keV, was considered within the framework of the modified potential cluster model (MPCM) with forbidden states and accounting for the resonance behavior of the scattering phase shifts. In the framework of the same model the possibility of describing the available experimental data for the total cross sections of the neutron radiative capture on 11B at thermal and astrophysical energies were considered with taking into account the 21 and 430 keV resonances. Description of the available experimental data on the total cross sections and astrophysical S-factor of the radiative proton capture on 11B to the ground state of 12C was treated at astrophysical energies. The possibility of description of the experimental data for the astrophysical S-factor of the radiative proton capture on 14C to the ground state of 15N at astrophysical energies, and the radiative proton capture on 15N at the energies from 50 to 1500 keV was considered in the framework of the MPCM with the classification of the orbital states according to Young tableaux. -
Energy Deposition by Neutrons
22.55 “Principles of Radiation Interactions” Neutrons Classification of neutrons by energy Thermal: E < 1 eV (0.025 eV) Epithermal: 1 eV < E < 10 keV Fast: > 10 keV Neutron sources Neutron energies Reactors neutrons in the few keV to several MeV Fusion reactions 14 MeV Large accelerators Hundreds of MeV Energy Deposition by Neutrons • Neutrons are generated over a wide range of energies by a variety of different processes. • Like photons, neutrons are uncharged and do not interact with orbital electrons. • Neutrons can travel considerable distances through matter without interacting. • Neutrons will interact with atomic nuclei through several mechanisms. o Elastic scatter o Inelastic scatter o Nonelastic scatter o Neutron capture o Spallation • The type of interaction depends on the neutron energy Radiation Interactions: neutrons Page 1 of 8 22.55 “Principles of Radiation Interactions” Cross Sections • Because mass attenuation coefficients, µ/ρ (cm2/g) have dimensions of cm2 in the numerator, they have come to be called “cross sections”. • Cross sections do not represent a physical area, but a probability of an interaction. • Cross sections usually expressed in the unit, barn: (10-24 cm2) • The atomic cross sections can be derived from the mass attenuation coefficient. Photons Cross sections are attenuation coefficients, expressed at the atom level (Probability of interaction per atom) ρ N = atom density (#atoms/cm3) N = N A A A 0 2 σA = atomic cross section (cm /atom) 23 N0 = 6.02 x 10 atoms/mole ρ = g/cm3 µ = N A σ A A = g/mole ρ µ = N σ A 0 A µ N σ ⎛ µ ⎞⎛ A ⎞ 0 A ⎜ ⎟⎜ ⎟ = σ A = ⎜ ⎟⎜ ⎟ ρ A ⎝ ρ ⎠⎝ N 0 ⎠ Radiation Interactions: neutrons Page 2 of 8 22.55 “Principles of Radiation Interactions” Neutron Cross Sections Analogous to photons • Neutrons interact by different mechanisms depending on the neutron energy and the material of the absorber o Scattering • elastic • inelastic o Capture • Each energy loss mechanism has a cross section • Neutron cross sections expressed in barns (1 barn = 10-24 cm2). -
Computing Neutron Capture Rates in Neutron-Degenerate Matter †
universe Article Computing Neutron Capture Rates in Neutron-Degenerate Matter † Bryn Knight and Liliana Caballero * Department of Physics, University of Guelph, Guelph, ON N1G 2W1, Canada; [email protected] * Correspondence: [email protected] † This paper is based on the talk at the 7th International Conference on New Frontiers in Physics (ICNFP 2018), Crete, Greece, 4–12 July 2018. Received: 28 November 2018; Accepted: 16 January 2019; Published: 18 January 2019 Abstract: Neutron captures are likely to occur in the crust of accreting neutron stars (NSs). Their rate depends on the thermodynamic state of neutrons in the crust. At high densities, neutrons are degenerate. We find degeneracy corrections to neutron capture rates off nuclei, using cross sections evaluated with the reaction code TALYS. We numerically integrate the relevant cross sections over the statistical distribution functions of neutrons at thermodynamic conditions present in the NS crust. We compare our results to analytical calculations of these corrections based on a power-law behavior of the cross section. We find that although an analytical integration can simplify the calculation and incorporation of the results for nucleosynthesis networks, there are uncertainties caused by departures of the cross section from the power-law approach at energies close to the neutron chemical potential. These deviations produce non-negligible corrections that can be important in the NS crust. Keywords: neutron capture; neutron stars; degenerate matter; nuclear reactions 1. Introduction X-ray burst and superburst observations are attributed to accreting neutron stars (NSs) (see, e.g., [1,2]). In such a scenario, a NS drags matter from a companion star. -
Neutron Capture Cross Sections of Cadmium Isotopes
Neutron Capture Cross Sections of Cadmium Isotopes By Allison Gicking A thesis submitted to Oregon State University In partial fulfillment of the requirements for the degree of Bachelor of Science Presented June 8, 2011 Commencement June 17, 2012 Abstract The neutron capture cross sections of 106Cd, 108Cd, 110Cd, 112Cd, 114Cd and 116Cd were determined in the present project. Four different OSU TRIGA reactor facilities were used to produce redundancy in the results and to measure the thermal cross section and resonance integral separately. When the present values were compared with previously measured values, the differences were mostly due to the kind of detector used or whether or not the samples were natural cadmium. Some of the isotopes did not have any previously measured values, and in that case, new information about the cross sections of those cadmium isotopes has been provided. Table of Contents I. Introduction………………………………………………………………….…….…1 II. Theory………………………………………………………………………...…...…3 1. Neutron Capture…………………………………………………….….……3 2. Resonance Integral vs. Effective Thermal Cross Section…………...………5 3. Derivation of the Activity Equations…………………………………....…..8 III. Methods………………………………………………………….................…...…...12 1. Irradiation of the Samples………………………………………….….....…12 2. Sample Preparation and Parameters………………..………...………..……16 3. Efficiency Calibration of Detectors…………………………..………....…..18 4. Data Analysis…………………………………...…….………………...…..19 5. Absorption by 113Cd……………………………………...……...….………20 IV. Results………………………………………………….……………..……….…….22 -
Nucleosynthetic Isotope Variations of Siderophile and Chalcophile
Reviews in Mineralogy & Geochemistry Vol.81 pp. 107-160, 2016 3 Copyright © Mineralogical Society of America Nucleosynthetic Isotope Variations of Siderophile and Chalcophile Elements in the Solar System Tetsuya Yokoyama Department of Earth and Planetary Sciences Tokyo Institute of Technology Ookayama, Tokyo 152-885 Japan [email protected] Richard J. Walker Department of Geology University of Maryland College Park, MD 20742 USA [email protected] INTRODUCTION Numerous investigations have been devoted to understanding how the materials that contributed to the Solar System formed, were incorporated into the precursor molecular cloud and the protoplanetary disk, and ultimately evolved into the building blocks of planetesimals and planets. Chemical and isotopic analyses of extraterrestrial materials have played a central role in decoding the signatures of individual processes that led to their formation. Among the elements studied, the siderophile and chalcophile elements are crucial for considering a range of formational and evolutionary processes. Consequently, over the past 60 years, considerable effort has been focused on the development of abundance and isotopic analyses of these elements in terrestrial and extraterrestrial materials (e.g., Shirey and Walker 1995; Birck et al. 1997; Reisberg and Meisel 2002; Meisel and Horan 2016, this volume). In this review, we consider nucleosynthetic isotopic variability of siderophile and chalcophile elements in meteorites. Chapter 4 provides a review for siderophile and chalcophile elements in planetary materials in general (Day et al. 2016, this volume). In many cases, such variability is denoted as an “isotopic anomaly”; however, the term can be ambiguous because several pre- and post- Solar System formation processes can lead to variability of isotopic compositions as recorded in meteorites.