An Introduction to Neutron Scattering
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Neutron Stars
Chandra X-Ray Observatory X-Ray Astronomy Field Guide Neutron Stars Ordinary matter, or the stuff we and everything around us is made of, consists largely of empty space. Even a rock is mostly empty space. This is because matter is made of atoms. An atom is a cloud of electrons orbiting around a nucleus composed of protons and neutrons. The nucleus contains more than 99.9 percent of the mass of an atom, yet it has a diameter of only 1/100,000 that of the electron cloud. The electrons themselves take up little space, but the pattern of their orbit defines the size of the atom, which is therefore 99.9999999999999% Chandra Image of Vela Pulsar open space! (NASA/PSU/G.Pavlov et al. What we perceive as painfully solid when we bump against a rock is really a hurly-burly of electrons moving through empty space so fast that we can't see—or feel—the emptiness. What would matter look like if it weren't empty, if we could crush the electron cloud down to the size of the nucleus? Suppose we could generate a force strong enough to crush all the emptiness out of a rock roughly the size of a football stadium. The rock would be squeezed down to the size of a grain of sand and would still weigh 4 million tons! Such extreme forces occur in nature when the central part of a massive star collapses to form a neutron star. The atoms are crushed completely, and the electrons are jammed inside the protons to form a star composed almost entirely of neutrons. -
The Five Common Particles
The Five Common Particles The world around you consists of only three particles: protons, neutrons, and electrons. Protons and neutrons form the nuclei of atoms, and electrons glue everything together and create chemicals and materials. Along with the photon and the neutrino, these particles are essentially the only ones that exist in our solar system, because all the other subatomic particles have half-lives of typically 10-9 second or less, and vanish almost the instant they are created by nuclear reactions in the Sun, etc. Particles interact via the four fundamental forces of nature. Some basic properties of these forces are summarized below. (Other aspects of the fundamental forces are also discussed in the Summary of Particle Physics document on this web site.) Force Range Common Particles It Affects Conserved Quantity gravity infinite neutron, proton, electron, neutrino, photon mass-energy electromagnetic infinite proton, electron, photon charge -14 strong nuclear force ≈ 10 m neutron, proton baryon number -15 weak nuclear force ≈ 10 m neutron, proton, electron, neutrino lepton number Every particle in nature has specific values of all four of the conserved quantities associated with each force. The values for the five common particles are: Particle Rest Mass1 Charge2 Baryon # Lepton # proton 938.3 MeV/c2 +1 e +1 0 neutron 939.6 MeV/c2 0 +1 0 electron 0.511 MeV/c2 -1 e 0 +1 neutrino ≈ 1 eV/c2 0 0 +1 photon 0 eV/c2 0 0 0 1) MeV = mega-electron-volt = 106 eV. It is customary in particle physics to measure the mass of a particle in terms of how much energy it would represent if it were converted via E = mc2. -
Fundamentals of Particle Physics
Fundamentals of Par0cle Physics Particle Physics Masterclass Emmanuel Olaiya 1 The Universe u The universe is 15 billion years old u Around 150 billion galaxies (150,000,000,000) u Each galaxy has around 300 billion stars (300,000,000,000) u 150 billion x 300 billion stars (that is a lot of stars!) u That is a huge amount of material u That is an unimaginable amount of particles u How do we even begin to understand all of matter? 2 How many elementary particles does it take to describe the matter around us? 3 We can describe the material around us using just 3 particles . 3 Matter Particles +2/3 U Point like elementary particles that protons and neutrons are made from. Quarks Hence we can construct all nuclei using these two particles -1/3 d -1 Electrons orbit the nuclei and are help to e form molecules. These are also point like elementary particles Leptons We can build the world around us with these 3 particles. But how do they interact. To understand their interactions we have to introduce forces! Force carriers g1 g2 g3 g4 g5 g6 g7 g8 The gluon, of which there are 8 is the force carrier for nuclear forces Consider 2 forces: nuclear forces, and electromagnetism The photon, ie light is the force carrier when experiencing forces such and electricity and magnetism γ SOME FAMILAR THE ATOM PARTICLES ≈10-10m electron (-) 0.511 MeV A Fundamental (“pointlike”) Particle THE NUCLEUS proton (+) 938.3 MeV neutron (0) 939.6 MeV E=mc2. Einstein’s equation tells us mass and energy are equivalent Wave/Particle Duality (Quantum Mechanics) Einstein E -
Photons from 252Cf and 241Am-Be Neutron Sources H
Neutronenbestrahlungsraum Calibration Laboratory LB6411 Am-Be Quelle [email protected] Photons from 252Cf and 241Am-Be neutron sources H. Hoedlmoser, M. Boschung, K. Meier and S. Mayer Paul Scherrer Institut, CH-5232 Villigen PSI, Switzerland At the accredited PSI calibration laboratory neutron reference fields traceable to the standards of the Physikalisch-Technische Bundesanstalt (PTB) in Germany are available for the calibration of ambient and personal dose equivalent (rate) meters and passive dosimeters. The photon contribution to H*(10) in the neutron fields of the 252Cf and 241Am-Be sources was measured using various photon dose rate meters and active and passive dosimeters. Measuring photons from a neutron source involves considerable uncertainties due to the presence of neutrons, due to a non-zero neutron sensitivity of the photon detector and due to the energy response of the photon detectors. Therefore eight independent detectors and methods were used to obtain a reliable estimate for the photon contribution as an average of the individual methods. For the 241Am-Be source a photon contribution of approximately 4.9% was determined and for the 252Cf source a contribution of 3.6%. 1) Photon detectors 2) Photons from 252Cf and 241Am-Be neutron sources Figure 1 252Cf decays through -emission (~97%) and through spontaneous fission (~3%) with a half-life of 2.65 y. Both processes are accompanied by photon radiation. Furthermore the spectrum of fission products contains radioactive elements that produce additional gamma photons. In the 241Am-Be source 241Am decays through -emission and various low energy emissions: 241Am237Np + + with a half life of 432.6 y. -
Neutron Instrumentation
Neutron Instrumentation Oxford School on Neutron Scattering 5th September 2019 Ken Andersen Summary • Neutron instrument concepts – time-of-flight – Bragg’s law • Neutron Instrumentation – guides – monochromators – shielding – detectors – choppers – sample environment – collimation • Neutron diffractometers • Neutron spectrometers 2 The time-of-flight (TOF) method distance Δt time Diffraction: Bragg’s Law Diffraction: Bragg’s Law Diffraction: Bragg’s Law Diffraction: Bragg’s Law Diffraction: Bragg’s Law Diffraction: Bragg’s Law λ = 2d sinθ Diffraction: Bragg’s Law λ = 2d sinθ 2θ Reflection: Snell’s Law incident reflected n=1 θ θ’ refracted n’<1 Reflection: Snell’s Law incident reflected n=1 θ θ’ refracted θ’=0: critical angle of total n’<1 reflection θc Reflection: Snell’s Law incident reflected n=1 θ θ’ refracted θ’=0: critical angle of total n’<1 reflection θc cosθc = n' n = n' Nλ2b n' = 1− ⇒ θc = λ Nb/π 2π ≈ − 2 cosθc 1 θc 2 Reflection: Snell’s Law incident reflected n=1 θ θ’ refracted θ’=0: critical angle of total n’<1 reflection θc cosθc = n' n = n' 2 for natural Ni, Nλ b n' = 1− ⇒ θc = λ Nb/π 2π θc = λ[Å]×0.1° cosθ ≈ 1− θ2 2 c c -1 Qc = 0.0218 Å Neutron Supermirrors Courtesy of J. Stahn, PSI Neutron Supermirrors Courtesy of J. Stahn, PSI Neutron Supermirrors Courtesy of J. Stahn, PSI Neutron Supermirrors λ Reflection: θc(Ni) = λ[Å] × 0.10° c λ 1 Multilayer: θc(SM) = m × λ[Å] × 0.10° λ 2 λ 3 λ 4 } d 1 } d 2 } d3 } d4 18 Neutron Supermirrors λ Reflection: θc(Ni) = λ[Å] × 0.10° c λ 1 Multilayer: θc(SM) = m × λ[Å] × 0.10° λ 2 -
Resolution Neutron Scattering Technique Using Triple-Axis
1 High -resolution neutron scattering technique using triple-axis spectrometers ¢ ¡ ¡ GUANGYONG XU, ¡ * P. M. GEHRING, V. J. GHOSH AND G. SHIRANE ¢ ¡ Physics Department, Brookhaven National Laboratory, Upton, NY 11973, and NCNR, National Institute of Standards and Technology, Gaithersburg, Maryland, 20899. E-mail: [email protected] (Received 0 XXXXXXX 0000; accepted 0 XXXXXXX 0000) Abstract We present a new technique which brings a substantial increase of the wave-vector £ - resolution of triple-axis-spectrometers by matching the measurement wave-vector £ to the ¥§¦©¨ reflection ¤ of a perfect crystal analyzer. A relative Bragg width of can be ¡ achieved with reasonable collimation settings. This technique is very useful in measuring small structural changes and line broadenings that can not be accurately measured with con- ventional set-ups, while still keeping all the strengths of a triple-axis-spectrometer. 1. Introduction Triple-axis-spectrometers (TAS) are widely used in both elastic and inelastic neutron scat- tering measurements to study the structures and dynamics in condensed matter. It has the £ flexibility to allow one to probe nearly all coordinates in energy ( ) and momentum ( ) space in a controlled manner, and the data can be easily interpreted (Bacon, 1975; Shirane et al., 2002). The resolution of a triple-axis-spectrometer is determined by many factors, including the ¨ incident (E ) and final (E ) neutron energies, the wave-vector transfer , the monochromator PREPRINT: Acta Crystallographica Section A A Journal of the International Union of Crystallography 2 and analyzer mosaic, and the beam collimations, etc. This has been studied in detail by Cooper & Nathans (1967), Werner & Pynn (1971) and Chesser & Axe (1973). -
The Theoretical Foundation of Spin-Echo Small-Angle Neutron
The Theoretical Foundation of Spin‐Echo Small‐Angle Neutron Scattering (SESANS) Applied in Colloidal System Wei‐Ren Chen, Gregory S. Smith, and Kenneth W. Herwig (NSSD ORNL) Yun Liu (NCNR NIST & Chemistry, University of Delaware) Li (Emily) Liu (Nuclear Engineering, RPI) Xin Li, Roger Pynn (Physics, Indiana University) Chwen‐Yang Shew (Chemistry, CUNY) UCANS‐II Indiana University July 08th 2011 Bloomington, IN Outline 1. Motivation — why Spin-Echo Small-Angle Neutron Scattering (SESANS)? 2. Basic Theory — what does SESANS measure? 3. Results and Discussions — what can SESANS do? (1). Straightforward observation of potential (2). Sensitivity to the local structure (3). Sensitivity to the structural heterogeneity 4. Summary Outline 1. Motivation — why Spin-Echo Small-Angle Neutron Scattering (SESANS)? 2. Basic Theory — what does SESANS measure? 3. Results and Discussions — what can SESANS do? (1). Straightforward observation of potential (2). Sensitivity to the local structure (3). Sensitivity to the structural heterogeneity 4. Summary Neutron Scattering Structure (Elastic Scatt.) Dynamics (Inelastic Scatt.) Small‐Angle Neutron Quasi‐Elastic Neutron Unpolarized Scattering (SANS), Scattering (QENS), beam Neutron Diffraction, Inelastic Neutron Scattering Neutron Reflectometry (INS) Polarized Spin‐Echo Small‐Angle Neutron Spin‐Echo (NSE) beam Neutron Scattering (SESANS) Neutron Scattering Structure (Elastic Scatt.) Dynamics (Inelastic Scatt.) Small‐Angle Neutron Quasi‐Elastic Neutron Unpolarized Scattering (SANS), Scattering (QENS), beam Neutron -
Neutron-Induced Fission Cross Section of 240,242Pu up to En = 3 Mev
Neutron-induced fission cross section of 240;242Pu Paula Salvador-Castineira~ Supervisors: Dr. Franz-Josef Hambsch Dr. Carme Pretel Doctoral dissertation PhD in Nuclear Engineering and Ionizing Radiation Barcelona, September 2014 Curs acadèmic: Acta de qualificació de tesi doctoral Nom i cognoms Programa de doctorat Unitat estructural responsable del programa Resolució del Tribunal Reunit el Tribunal designat a l'efecte, el doctorand / la doctoranda exposa el tema de la seva tesi doctoral titulada __________________________________________________________________________________________ _________________________________________________________________________________________. Acabada la lectura i després de donar resposta a les qüestions formulades pels membres titulars del tribunal, aquest atorga la qualificació: NO APTE APROVAT NOTABLE EXCEL·LENT (Nom, cognoms i signatura) (Nom, cognoms i signatura) President/a Secretari/ària (Nom, cognoms i signatura) (Nom, cognoms i signatura) (Nom, cognoms i signatura) Vocal Vocal Vocal ______________________, _______ d'/de __________________ de _______________ El resultat de l’escrutini dels vots emesos pels membres titulars del tribunal, efectuat per l’Escola de Doctorat, a instància de la Comissió de Doctorat de la UPC, atorga la MENCIÓ CUM LAUDE: SÍ NO (Nom, cognoms i signatura) (Nom, cognoms i signatura) President de la Comissió Permanent de l’Escola de Doctorat Secretària de la Comissió Permanent de l’Escola de Doctorat Barcelona, _______ d'/de ____________________ de _________ Universitat Politecnica` -
Part B. Radiation Sources Radiation Safety
Part B. Radiation sources Radiation Safety 1. Interaction of electrons-e with the matter −31 me = 9.11×10 kg ; E = m ec2 = 0.511 MeV; qe = -e 2. Interaction of photons-γ with the matter mγ = 0 kg ; E γ = 0 eV; q γ = 0 3. Interaction of neutrons-n with the matter −27 mn = 1.68 × 10 kg ; En = 939.57 MeV; qn = 0 4. Interaction of protons-p with the matter −27 mp = 1.67 × 10 kg ; Ep = 938.27 MeV; qp = +e Note: for any nucleus A: mass number – nucleons number A = Z + N Z: atomic number – proton (charge) number N: neutron number 1 / 35 1. Interaction of electrons with the matter Radiation Safety The physical processes: 1. Ionization losses inelastic collisions with orbital electrons 2. Bremsstrahlung losses inelastic collisions with atomic nuclei 3. Rutherford scattering elastic collisions with atomic nuclei Positrons at nearly rest energy: annihilation emission of two 511 keV photons 2 / 35 1. Interaction of electrons with1.E+02 the matter Radiation Safety ) 1.E+03 -1 Graphite – Z = 6 .g 2 1.E+01 ) Lead – Z = 82 -1 .g 2 1.E+02 1.E+00 1.E+01 1.E-01 1.E+00 collision 1.E-02 radiative collision 1.E-01 stopping pow er (MeV.cm total radiative 1.E-03 stopping pow er (MeV.cm total 1.E-02 1.E-01 1.E+00 1.E+01 1.E+02 1.E+03 1.E-02 energy (MeV) 1.E-02 1.E-01 1.E+00 1.E+01 1.E+02 1.E+03 Electrons – stopping power 1.E+02 energy (MeV) S 1 dE ) === -1 Copper – Z = 29 ρρρ ρρρ dl .g 2 1.E+01 S 1 dE 1 dE === +++ ρρρ ρρρ dl coll ρρρ dl rad 1 dE 1.E+00 : mass stopping power (MeV.cm 2 g. -
Neutron Scattering
Neutron Scattering John R.D. Copley Summer School on Methods and Applications of High Resolution Neutron Spectroscopy and Small Angle Neutron Scattering NIST Center for NeutronNCNR Summer Research, School 2011 June 12-16, 2011 Acknowledgements National Science Foundation NIST Center for Neutron (grant # DMR-0944772) Research (NCNR) Center for High Resolution Neutron Scattering (CHRNS) 2 NCNR Summer School 2011 (Slow) neutron interactions Scattering plus Absorption Total =+Elastic Inelastic scattering scattering scattering (diffraction) (spectroscopy) includes “Quasielastic neutron Structure Dynamics scattering” (QENS) NCNR Summer School 2011 3 Total, elastic, and inelastic scattering Incident energy Ei E= Ei -Ef Scattered energy Ef (“energy transfer”) Total scattering: Elastic scattering: E = E (i.e., E = 0) all Ef (i.e., all E) f i Inelastic scattering: E ≠ E (i.e., E ≠ 0) D f i A M M Ef Ei S Ei D S Diffractometer Spectrometer (Some write E = Ef –Ei) NCNR Summer School 2011 4 Kinematics mv= = k 1 222 Emvk2m==2 = Scattered wave (m is neutron’s mass) vector k , energy E 2θ f f Incident wave vector ki, energy Ei N.B. The symbol for scattering angle in Q is wave vector transfer, SANS experiments is or “scattering vector” Q =Q is momentum transfer θ, not 2θ. Q = ki - kf (For x-rays, Eck = = ) (“wave vector transfer”) NCNR Summer School 2011 5 Elastic scattering Q = ki - kf G In real space k In reciprocal space f G G G kf Q ki 2θ 2θ G G k Q i E== 0 kif k Q =θ 2k i sin NCNR Summer School 2011 6 Total scattering, inelastic scattering Q = ki - kf G kf G Q Qkk2kkcos2222= +− θ 2θ G if if ki At fixed scattering angle 2θ, the magnitude (and the direction) of Q varies with the energy transfer E. -
Probing the Minimal Length Scale by Precision Tests of the Muon G − 2
Physics Letters B 584 (2004) 109–113 www.elsevier.com/locate/physletb Probing the minimal length scale by precision tests of the muon g − 2 U. Harbach, S. Hossenfelder, M. Bleicher, H. Stöcker Institut für Theoretische Physik, J.W. Goethe-Universität, Robert-Mayer-Str. 8-10, 60054 Frankfurt am Main, Germany Received 25 November 2003; received in revised form 20 January 2004; accepted 21 January 2004 Editor: P.V. Landshoff Abstract Modifications of the gyromagnetic moment of electrons and muons due to a minimal length scale combined with a modified fundamental scale Mf are explored. First-order deviations from the theoretical SM value for g − 2 due to these string theory- motivated effects are derived. Constraints for the fundamental scale Mf are given. 2004 Elsevier B.V. All rights reserved. String theory suggests the existence of a minimum • the need for a higher-dimensional space–time and length scale. An exciting quantum mechanical impli- • the existence of a minimal length scale. cation of this feature is a modification of the uncer- tainty principle. In perturbative string theory [1,2], Naturally, this minimum length uncertainty is re- the feature of a fundamental minimal length scale lated to a modification of the standard commutation arises from the fact that strings cannot probe dis- relations between position and momentum [6,7]. Ap- tances smaller than the string scale. If the energy of plication of this is of high interest for quantum fluc- a string reaches the Planck mass mp, excitations of the tuations in the early universe and inflation [8–16]. string can occur and cause a non-zero extension [3]. -
The Basic Interactions Between Photons and Charged Particles With
Outline Chapter 6 The Basic Interactions between • Photon interactions Photons and Charged Particles – Photoelectric effect – Compton scattering with Matter – Pair productions Radiation Dosimetry I – Coherent scattering • Charged particle interactions – Stopping power and range Text: H.E Johns and J.R. Cunningham, The – Bremsstrahlung interaction th physics of radiology, 4 ed. – Bragg peak http://www.utoledo.edu/med/depts/radther Photon interactions Photoelectric effect • Collision between a photon and an • With energy deposition atom results in ejection of a bound – Photoelectric effect electron – Compton scattering • The photon disappears and is replaced by an electron ejected from the atom • No energy deposition in classical Thomson treatment with kinetic energy KE = hν − Eb – Pair production (above the threshold of 1.02 MeV) • Highest probability if the photon – Photo-nuclear interactions for higher energies energy is just above the binding energy (above 10 MeV) of the electron (absorption edge) • Additional energy may be deposited • Without energy deposition locally by Auger electrons and/or – Coherent scattering Photoelectric mass attenuation coefficients fluorescence photons of lead and soft tissue as a function of photon energy. K and L-absorption edges are shown for lead Thomson scattering Photoelectric effect (classical treatment) • Electron tends to be ejected • Elastic scattering of photon (EM wave) on free electron o at 90 for low energy • Electron is accelerated by EM wave and radiates a wave photons, and approaching • No