X-Ray Scattering by a Free Electron
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Glossary Physics (I-Introduction)
1 Glossary Physics (I-introduction) - Efficiency: The percent of the work put into a machine that is converted into useful work output; = work done / energy used [-]. = eta In machines: The work output of any machine cannot exceed the work input (<=100%); in an ideal machine, where no energy is transformed into heat: work(input) = work(output), =100%. Energy: The property of a system that enables it to do work. Conservation o. E.: Energy cannot be created or destroyed; it may be transformed from one form into another, but the total amount of energy never changes. Equilibrium: The state of an object when not acted upon by a net force or net torque; an object in equilibrium may be at rest or moving at uniform velocity - not accelerating. Mechanical E.: The state of an object or system of objects for which any impressed forces cancels to zero and no acceleration occurs. Dynamic E.: Object is moving without experiencing acceleration. Static E.: Object is at rest.F Force: The influence that can cause an object to be accelerated or retarded; is always in the direction of the net force, hence a vector quantity; the four elementary forces are: Electromagnetic F.: Is an attraction or repulsion G, gravit. const.6.672E-11[Nm2/kg2] between electric charges: d, distance [m] 2 2 2 2 F = 1/(40) (q1q2/d ) [(CC/m )(Nm /C )] = [N] m,M, mass [kg] Gravitational F.: Is a mutual attraction between all masses: q, charge [As] [C] 2 2 2 2 F = GmM/d [Nm /kg kg 1/m ] = [N] 0, dielectric constant Strong F.: (nuclear force) Acts within the nuclei of atoms: 8.854E-12 [C2/Nm2] [F/m] 2 2 2 2 2 F = 1/(40) (e /d ) [(CC/m )(Nm /C )] = [N] , 3.14 [-] Weak F.: Manifests itself in special reactions among elementary e, 1.60210 E-19 [As] [C] particles, such as the reaction that occur in radioactive decay. -
High-Energy Astrophysics
High-Energy Astrophysics Andrii Neronov October 30, 2017 2 Contents 1 Introduction 5 1.1 Types of astronomical HE sources . .7 1.2 Types of physical processes involved . .8 1.3 Observational tools . .9 1.4 Natural System of Units . 11 1.5 Excercises . 14 2 Radiative Processes 15 2.1 Radiation from a moving charge . 15 2.2 Curvature radiation . 17 2.2.1 Astrophysical example (pulsar magnetosphere) . 19 2.3 Evolution of particle distribution with account of radiative energy loss . 20 2.4 Spectrum of emission from a broad-band distribution of particles . 21 2.5 Cyclotron emission / absorption . 23 2.5.1 Astrophysical example (accreting pulsars) . 23 2.6 Synchrotron emission . 24 2.6.1 Astrophysical example (Crab Nebula) . 26 2.7 Compton scattering . 28 2.7.1 Thomson cross-section . 28 2.7.2 Example: Compton scattering in stars. Optical depth of the medium. Eddington luminosity 30 2.7.3 Angular distribution of scattered waves . 31 2.7.4 Thomson scattering . 32 2.7.5 Example: Compton telescope(s) . 33 2.8 Inverse Compton scattering . 34 2.8.1 Energies of upscattered photons . 34 2.8.2 Energy loss rate of electron . 35 2.8.3 Evolution of particle distribution with account of radiative energy loss . 36 2.8.4 Spectrum of emission from a broad-band distribution of particles . 36 2.8.5 Example: Very-High-Energy gamma-rays from Crab Nebula . 37 2.8.6 Inverse Compton scattering in Klein-Nishina regime . 37 2.9 Bethe-Heitler pair production . 38 2.9.1 Example: pair conversion telescopes. -
A CMB Polarization Primer
New Astronomy 2 (1997) 323±344 A CMB polarization primer Wayne Hua,1,2 , Martin White b,3 aInstitute for Advanced Study, Princeton, NJ 08540, USA bEnrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA Received 13 June 1997; accepted 30 June 1997 Communicated by David N. Schramm Abstract We present a pedagogical and phenomenological introduction to the study of cosmic microwave background (CMB) polarization to build intuition about the prospects and challenges facing its detection. Thomson scattering of temperature anisotropies on the last scattering surface generates a linear polarization pattern on the sky that can be simply read off from their quadrupole moments. These in turn correspond directly to the fundamental scalar (compressional), vector (vortical), and tensor (gravitational wave) modes of cosmological perturbations. We explain the origin and phenomenology of the geometric distinction between these patterns in terms of the so-called electric and magnetic parity modes, as well as their correlation with the temperature pattern. By its isolation of the last scattering surface and the various perturbation modes, the polarization provides unique information for the phenomenological reconstruction of the cosmological model. Finally we comment on the comparison of theory with experimental data and prospects for the future detection of CMB polarization. 1997 Elsevier Science B.V. PACS: 98.70.Vc; 98.80.Cq; 98.80.Es Keywords: Cosmic microwave background; Cosmology: theory 1. Introduction scale structure we see today. If the temperature anisotropies we observe are indeed the result of Why should we be concerned with the polarization primordial ¯uctuations, their presence at last scatter- of the cosmic microwave background (CMB) ing would polarize the CMB anisotropies them- anisotropies? That the CMB anisotropies are polar- selves. -
12 Light Scattering AQ1
12 Light Scattering AQ1 Lev T. Perelman CONTENTS 12.1 Introduction ......................................................................................................................... 321 12.2 Basic Principles of Light Scattering ....................................................................................323 12.3 Light Scattering Spectroscopy ............................................................................................325 12.4 Early Cancer Detection with Light Scattering Spectroscopy .............................................326 12.5 Confocal Light Absorption and Scattering Spectroscopic Microscopy ............................. 329 12.6 Light Scattering Spectroscopy of Single Nanoparticles ..................................................... 333 12.7 Conclusions ......................................................................................................................... 335 Acknowledgment ........................................................................................................................... 335 References ...................................................................................................................................... 335 12.1 INTRODUCTION Light scattering in biological tissues originates from the tissue inhomogeneities such as cellular organelles, extracellular matrix, blood vessels, etc. This often translates into unique angular, polari- zation, and spectroscopic features of scattered light emerging from tissue and therefore information about tissue -
Solutions 7: Interacting Quantum Field Theory: Λφ4
QFT PS7 Solutions: Interacting Quantum Field Theory: λφ4 (4/1/19) 1 Solutions 7: Interacting Quantum Field Theory: λφ4 Matrix Elements vs. Green Functions. Physical quantities in QFT are derived from matrix elements M which represent probability amplitudes. Since particles are characterised by having a certain three momentum and a mass, and hence a specified energy, we specify such physical calculations in terms of such \on-shell" values i.e. four-momenta where p2 = m2. For instance the notation in momentum space for a ! scattering in scalar Yukawa theory uses four-momenta labels p1 and p2 flowing into the diagram for initial states, with q1 and q2 flowing out of the diagram for the final states, all of which are on-shell. However most manipulations in QFT, and in particular in this problem sheet, work with Green func- tions not matrix elements. Green functions are defined for arbitrary values of four momenta including unphysical off-shell values where p2 6= m2. So much of the information encoded in a Green function has no obvious physical meaning. Of course to extract the corresponding physical matrix element from the Greens function we would have to apply such physical constraints in order to get the physics of scattering of real physical particles. Alternatively our Green function may be part of an analysis of a much bigger diagram so it represents contributions from virtual particles to some more complicated physical process. ∗1. The full propagator in λφ4 theory Consider a theory of a real scalar field φ 1 1 λ L = (@ φ)(@µφ) − m2φ2 − φ4 (1) 2 µ 2 4! (i) A theory with a gφ3=(3!) interaction term will not have an energy which is bounded below. -
Arxiv:2008.11688V1 [Astro-Ph.CO] 26 Aug 2020
APS/123-QED Cosmology with Rayleigh Scattering of the Cosmic Microwave Background Benjamin Beringue,1 P. Daniel Meerburg,2 Joel Meyers,3 and Nicholas Battaglia4 1DAMTP, Centre for Mathematical Sciences, Wilberforce Road, Cambridge, UK, CB3 0WA 2Van Swinderen Institute for Particle Physics and Gravity, University of Groningen, Nijenborgh 4, 9747 AG Groningen, The Netherlands 3Department of Physics, Southern Methodist University, 3215 Daniel Ave, Dallas, Texas 75275, USA 4Department of Astronomy, Cornell University, Ithaca, New York, USA (Dated: August 27, 2020) The cosmic microwave background (CMB) has been a treasure trove for cosmology. Over the next decade, current and planned CMB experiments are expected to exhaust nearly all primary CMB information. To further constrain cosmological models, there is a great benefit to measuring signals beyond the primary modes. Rayleigh scattering of the CMB is one source of additional cosmological information. It is caused by the additional scattering of CMB photons by neutral species formed during recombination and exhibits a strong and unique frequency scaling ( ν4). We will show that with sufficient sensitivity across frequency channels, the Rayleigh scattering/ signal should not only be detectable but can significantly improve constraining power for cosmological parameters, with limited or no additional modifications to planned experiments. We will provide heuristic explanations for why certain cosmological parameters benefit from measurement of the Rayleigh scattering signal, and confirm these intuitions using the Fisher formalism. In particular, observation of Rayleigh scattering P allows significant improvements on measurements of Neff and mν . PACS numbers: Valid PACS appear here I. INTRODUCTION direction of propagation of the (primary) CMB photons. There are various distinguishable ways that cosmic In the current era of precision cosmology, the Cosmic structures can alter the properties of CMB photons [10]. -
The Cosmic Microwave Background: the History of Its Experimental Investigation and Its Significance for Cosmology
REVIEW ARTICLE The Cosmic Microwave Background: The history of its experimental investigation and its significance for cosmology Ruth Durrer Universit´ede Gen`eve, D´epartement de Physique Th´eorique,1211 Gen`eve, Switzerland E-mail: [email protected] Abstract. This review describes the discovery of the cosmic microwave background radiation in 1965 and its impact on cosmology in the 50 years that followed. This discovery has established the Big Bang model of the Universe and the analysis of its fluctuations has confirmed the idea of inflation and led to the present era of precision cosmology. I discuss the evolution of cosmological perturbations and their imprint on the CMB as temperature fluctuations and polarization. I also show how a phase of inflationary expansion generates fluctuations in the spacetime curvature and primordial gravitational waves. In addition I present findings of CMB experiments, from the earliest to the most recent ones. The accuracy of these experiments has helped us to estimate the parameters of the cosmological model with unprecedented precision so that in the future we shall be able to test not only cosmological models but General Relativity itself on cosmological scales. Submitted to: Class. Quantum Grav. arXiv:1506.01907v1 [astro-ph.CO] 5 Jun 2015 The Cosmic Microwave Background 2 1. Historical Introduction The discovery of the Cosmic Microwave Background (CMB) by Penzias and Wilson, reported in Refs. [1, 2], has been a 'game changer' in cosmology. Before this discovery, despite the observation of the expansion of the Universe, see [3], the steady state model of cosmology still had a respectable group of followers. -
Electron-Positron Pairs in Physics and Astrophysics
Electron-positron pairs in physics and astrophysics: from heavy nuclei to black holes Remo Ruffini1,2,3, Gregory Vereshchagin1 and She-Sheng Xue1 1 ICRANet and ICRA, p.le della Repubblica 10, 65100 Pescara, Italy, 2 Dip. di Fisica, Universit`adi Roma “La Sapienza”, Piazzale Aldo Moro 5, I-00185 Roma, Italy, 3 ICRANet, Universit´ede Nice Sophia Antipolis, Grand Chˆateau, BP 2135, 28, avenue de Valrose, 06103 NICE CEDEX 2, France. Abstract Due to the interaction of physics and astrophysics we are witnessing in these years a splendid synthesis of theoretical, experimental and observational results originating from three fundamental physical processes. They were originally proposed by Dirac, by Breit and Wheeler and by Sauter, Heisenberg, Euler and Schwinger. For almost seventy years they have all three been followed by a continued effort of experimental verification on Earth-based experiments. The Dirac process, e+e 2γ, has been by − → far the most successful. It has obtained extremely accurate experimental verification and has led as well to an enormous number of new physics in possibly one of the most fruitful experimental avenues by introduction of storage rings in Frascati and followed by the largest accelerators worldwide: DESY, SLAC etc. The Breit–Wheeler process, 2γ e+e , although conceptually simple, being the inverse process of the Dirac one, → − has been by far one of the most difficult to be verified experimentally. Only recently, through the technology based on free electron X-ray laser and its numerous applications in Earth-based experiments, some first indications of its possible verification have been reached. The vacuum polarization process in strong electromagnetic field, pioneered by Sauter, Heisenberg, Euler and Schwinger, introduced the concept of critical electric 2 3 field Ec = mec /(e ). -
1.3.4 Atoms and Molecules Name Symbol Definition SI Unit
1.3.4 Atoms and molecules Name Symbol Definition SI unit Notes nucleon number, A 1 mass number proton number, Z 1 atomic number neutron number N N = A - Z 1 electron rest mass me kg (1) mass of atom, ma, m kg atomic mass 12 atomic mass constant mu mu = ma( C)/12 kg (1), (2) mass excess ∆ ∆ = ma - Amu kg elementary charge, e C proton charage Planck constant h J s Planck constant/2π h h = h/2π J s 2 2 Bohr radius a0 a0 = 4πε0 h /mee m -1 Rydberg constant R∞ R∞ = Eh/2hc m 2 fine structure constant α α = e /4πε0 h c 1 ionization energy Ei J electron affinity Eea J (1) Analogous symbols are used for other particles with subscripts: p for proton, n for neutron, a for atom, N for nucleus, etc. (2) mu is equal to the unified atomic mass unit, with symbol u, i.e. mu = 1 u. In biochemistry the name dalton, with symbol Da, is used for the unified atomic mass unit, although the name and symbols have not been accepted by CGPM. Chapter 1 - 1 Name Symbol Definition SI unit Notes electronegativity χ χ = ½(Ei +Eea) J (3) dissociation energy Ed, D J from the ground state D0 J (4) from the potential De J (4) minimum principal quantum n E = -hcR/n2 1 number (H atom) angular momentum see under Spectroscopy, section 3.5. quantum numbers -1 magnetic dipole m, µ Ep = -m⋅⋅⋅B J T (5) moment of a molecule magnetizability ξ m = ξB J T-2 of a molecule -1 Bohr magneton µB µB = eh/2me J T (3) The concept of electronegativity was intoduced by L. -
Arxiv:1706.03391V2 [Astro-Ph.CO] 12 Sep 2017
Insights into neutrino decoupling gleaned from considerations of the role of electron mass E. Grohs∗ Department of Physics, University of Michigan, Ann Arbor, Michigan 48109, USA George M. Fuller Department of Physics, University of California, San Diego, La Jolla, California 92093, USA Abstract We present calculations showing how electron rest mass influences entropy flow, neutrino decoupling, and Big Bang Nucleosynthesis (BBN) in the early universe. To elucidate this physics and especially the sensitivity of BBN and related epochs to electron mass, we consider a parameter space of rest mass values larger and smaller than the accepted vacuum value. Electromagnetic equilibrium, coupled with the high entropy of the early universe, guarantees that significant numbers of electron-positron pairs are present, and dominate over the number of ionization electrons to temperatures much lower than the vacuum electron rest mass. Scattering between the electrons-positrons and the neutrinos largely controls the flow of entropy from the plasma into the neu- trino seas. Moreover, the number density of electron-positron-pair targets can be exponentially sensitive to the effective in-medium electron mass. This en- tropy flow influences the phasing of scale factor and temperature, the charged current weak-interaction-determined neutron-to-proton ratio, and the spectral distortions in the relic neutrino energy spectra. Our calculations show the sen- sitivity of the physics of this epoch to three separate effects: finite electron mass, finite-temperature quantum electrodynamic (QED) effects on the plasma equation of state, and Boltzmann neutrino energy transport. The ratio of neu- trino to plasma-component energy scales manifests in Cosmic Microwave Back- ground (CMB) observables, namely the baryon density and the radiation energy density, along with the primordial helium and deuterium abundances. -
Thermal History FRW
Cosmology, lect. 7 Thermal History FRW Thermodynamics 43πGpΛ a =−++ρ aa To find solutions a(t) for the 33c2 expansion history of the Universe, for a particular FRW Universe , 8πG kc2 Λ one needs to know how the 22=ρ −+ 2density ρ(t) and pressure p(t) aa 2 aevolve as function of a(t) 33R0 FRW equations are implicitly equivalent to a third Einstein equation, the energy equation, pa ρρ ++30 = ca2 Important observation: the energy equation, pa ρρ ++30 = ca2 is equivalent to stating that the change in internal energy U= ρ cV2 of a specific co-expanding volume V(t) of the Universe, is due to work by pressure: dU= − p dV Friedmann-Robertson-Walker-Lemaitre expansion of the Universe is Adiabatic Expansion Adiabatic Expansion of the Universe: • Implication for Thermal History • Temperature Evolution of cosmic components For a medium with adiabatic index γ: TVγ −1 = cst 4 T Radiation (Photons) γ = T = 0 3 a T 5 = 0 Monatomic Gas γ = T 2 (hydrogen) 3 a Radiation & Matter The Universe is filled with thermal radiation, the photons that were created in The Big Bang and that we now observe as the Cosmic Microwave Background (CMB). The CMB photons represent the most abundant species in the Universe, by far ! The CMB radiation field is PERFECTLY thermalized, with their energy distribution representing the most perfect blackbody spectrum we know in nature. The energy density u(T) is therefore given by the Planck spectral distribution, 81πνh 3 uT()= ν ce3/hν kT −1 At present, the temperature T of the cosmic radiation field is known to impressive precision, -
Arxiv:2006.06594V1 [Astro-Ph.CO]
Mitigating the optical depth degeneracy using the kinematic Sunyaev-Zel'dovich effect with CMB-S4 1, 2, 2, 1, 3, 4, 5, 6, 5, 6, Marcelo A. Alvarez, ∗ Simone Ferraro, y J. Colin Hill, z Ren´eeHloˇzek, x and Margaret Ikape { 1Berkeley Center for Cosmological Physics, Department of Physics, University of California, Berkeley, CA 94720, USA 2Lawrence Berkeley National Laboratory, One Cyclotron Road, Berkeley, CA 94720, USA 3Department of Physics, Columbia University, New York, NY, USA 10027 4Center for Computational Astrophysics, Flatiron Institute, New York, NY, USA 10010 5Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto ON, M5S 3H4, Canada 6David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto ON, M5S 3H4, Canada The epoch of reionization is one of the major phase transitions in the history of the universe, and is a focus of ongoing and upcoming cosmic microwave background (CMB) experiments with im- proved sensitivity to small-scale fluctuations. Reionization also represents a significant contaminant to CMB-derived cosmological parameter constraints, due to the degeneracy between the Thomson- scattering optical depth, τ, and the amplitude of scalar perturbations, As. This degeneracy subse- quently hinders the ability of large-scale structure data to constrain the sum of the neutrino masses, a major target for cosmology in the 2020s. In this work, we explore the kinematic Sunyaev-Zel'dovich (kSZ) effect as a probe of reionization, and show that it can be used to mitigate the optical depth degeneracy with high-sensitivity, high-resolution data from the upcoming CMB-S4 experiment.