The Bohr Atom
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Physics of the Atom
Physics of the Atom Ernest The Nobel Prize in Chemistry 1908 Rutherford "for his investigations into the disintegration of the elements, and the chemistry of radioactive substances" Niels Bohr The Nobel Prize in Physics 1922 "for his services in the investigation of the structure of atoms and of the radiation emanating from them" W. Ubachs – Lectures MNW-1 Early models of the atom atoms : electrically neutral they can become charged positive and negative charges are around and some can be removed. popular atomic model “plum-pudding” model: W. Ubachs – Lectures MNW-1 Rutherford scattering Rutherford did an experiment that showed that the positively charged nucleus must be extremely small compared to the rest of the atom. Result from Rutherford scattering 2 dσ ⎛ 1 Zze2 ⎞ 1 = ⎜ ⎟ ⎜ ⎟ 4 dΩ ⎝ 4πε0 4K ⎠ sin ()θ / 2 Applet for doing the experiment: http://www.physics.upenn.edu/courses/gladney/phys351/classes/Scattering/Rutherford_Scattering.html W. Ubachs – Lectures MNW-1 Rutherford scattering the smallness of the nucleus the radius of the nucleus is 1/10,000 that of the atom. the atom is mostly empty space Rutherford’s atomic model W. Ubachs – Lectures MNW-1 Atomic Spectra: Key to the Structure of the Atom A very thin gas heated in a discharge tube emits light only at characteristic frequencies. W. Ubachs – Lectures MNW-1 Atomic Spectra: Key to the Structure of the Atom Line spectra: absorption and emission W. Ubachs – Lectures MNW-1 The Balmer series in atomic hydrogen The wavelengths of electrons emitted from hydrogen have a regular pattern: Johann Jakob Balmer W. Ubachs – Lectures MNW-1 Lyman, Paschen and Rydberg series the Lyman series: the Paschen series: W. -
Optical Properties of Bulk and Nano
Lecture 3: Optical Properties of Bulk and Nano 5 nm Course Info First H/W#1 is due Sept. 10 The Previous Lecture Origin frequency dependence of χ in real materials • Lorentz model (harmonic oscillator model) e- n(ω) n' n'' n'1= ω0 + Nucleus ω0 ω Today optical properties of materials • Insulators (Lattice absorption, color centers…) • Semiconductors (Energy bands, Urbach tail, excitons …) • Metals (Response due to bound and free electrons, plasma oscillations.. ) Optical properties of molecules, nanoparticles, and microparticles Classification Matter: Insulators, Semiconductors, Metals Bonds and bands • One atom, e.g. H. Schrödinger equation: E H+ • Two atoms: bond formation ? H+ +H Every electron contributes one state • Equilibrium distance d (after reaction) Classification Matter ~ 1 eV • Pauli principle: Only 2 electrons in the same electronic state (one spin & one spin ) Classification Matter Atoms with many electrons Empty outer orbitals Outermost electrons interact Form bands Partly filled valence orbitals Filled Energy Inner Electrons in inner shells do not interact shells Do not form bands Distance between atoms Classification Matter Insulators, semiconductors, and metals • Classification based on bandstructure Dispersion and Absorption in Insulators Electronic transitions No transitions Atomic vibrations Refractive Index Various Materials 3.4 3.0 2.0 Refractive index: n’ index: Refractive 1.0 0.1 1.0 10 λ (µm) Color Centers • Insulators with a large EGAP should not show absorption…..or ? • Ion beam irradiation or x-ray exposure result in beautiful colors! • Due to formation of color (absorption) centers….(Homework assignment) Absorption Processes in Semiconductors Absorption spectrum of a typical semiconductor E EC Phonon Photon EV ωPhonon Excitons: Electron and Hole Bound by Coulomb Analogy with H-atom • Electron orbit around a hole is similar to the electron orbit around a H-core • 1913 Niels Bohr: Electron restricted to well-defined orbits n = 1 + -13.6 eV n = 2 n = 3 -3.4 eV -1.51 eV me4 13.6 • Binding energy electron: =−=−=e EB 2 2 eV, n 1,2,3,.. -
Bohr Model of Hydrogen
Chapter 3 Bohr model of hydrogen Figure 3.1: Democritus The atomic theory of matter has a long history, in some ways all the way back to the ancient Greeks (Democritus - ca. 400 BCE - suggested that all things are composed of indivisible \atoms"). From what we can observe, atoms have certain properties and behaviors, which can be summarized as follows: Atoms are small, with diameters on the order of 0:1 nm. Atoms are stable, they do not spontaneously break apart into smaller pieces or collapse. Atoms contain negatively charged electrons, but are electrically neutral. Atoms emit and absorb electromagnetic radiation. Any successful model of atoms must be capable of describing these observed properties. 1 (a) Isaac Newton (b) Joseph von Fraunhofer (c) Gustav Robert Kirch- hoff 3.1 Atomic spectra Even though the spectral nature of light is present in a rainbow, it was not until 1666 that Isaac Newton showed that white light from the sun is com- posed of a continuum of colors (frequencies). Newton introduced the term \spectrum" to describe this phenomenon. His method to measure the spec- trum of light consisted of a small aperture to define a point source of light, a lens to collimate this into a beam of light, a glass spectrum to disperse the colors and a screen on which to observe the resulting spectrum. This is indeed quite close to a modern spectrometer! Newton's analysis was the beginning of the science of spectroscopy (the study of the frequency distri- bution of light from different sources). The first observation of the discrete nature of emission and absorption from atomic systems was made by Joseph Fraunhofer in 1814. -
Particle Nature of Matter
Solved Problems on the Particle Nature of Matter Charles Asman, Adam Monahan and Malcolm McMillan Department of Physics and Astronomy University of British Columbia, Vancouver, British Columbia, Canada Fall 1999; revised 2011 by Malcolm McMillan Given here are solutions to 5 problems on the particle nature of matter. The solutions were used as a learning-tool for students in the introductory undergraduate course Physics 200 Relativity and Quanta given by Malcolm McMillan at UBC during the 1998 and 1999 Winter Sessions. The solutions were prepared in collaboration with Charles Asman and Adam Monaham who were graduate students in the Department of Physics at the time. The problems are from Chapter 3 The Particle Nature of Matter of the course text Modern Physics by Raymond A. Serway, Clement J. Moses and Curt A. Moyer, Saunders College Publishing, 2nd ed., (1997). Coulomb's Constant and the Elementary Charge When solving numerical problems on the particle nature of matter it is useful to note that the product of Coulomb's constant k = 8:9876 × 109 m2= C2 (1) and the square of the elementary charge e = 1:6022 × 10−19 C (2) is ke2 = 1:4400 eV nm = 1:4400 keV pm = 1:4400 MeV fm (3) where eV = 1:6022 × 10−19 J (4) Breakdown of the Rutherford Scattering Formula: Radius of a Nucleus Problem 3.9, page 39 It is observed that α particles with kinetic energies of 13.9 MeV or higher, incident on copper foils, do not obey Rutherford's (sin φ/2)−4 scattering formula. • Use this observation to estimate the radius of the nucleus of a copper atom. -
Bohr's Theory and Spectra of Hydrogen And
____________________________________________________________________________________________________ Subject Chemistry Paper No and Title 8 and Physical Spectroscopy Module No and Title 7 and Bohr’s theory and spectra of hydrogen and hydrogen- like ions. Module Tag CHE_P8_M7 CHEMISTRY PAPER No. : 8 (PHYSICAL SPECTROSCOPY) MODULE No. : 7 (BOHR’S THEORY AND SPECTRA OF HYDROGEN AND HYDROGEN-LIKE IONS) ____________________________________________________________________________________________________ TABLE OF CONTENTS 1. Learning Outcomes 2. What is a Spectrum? 2.1 Introduction 2.2 Atomic Spectra 2.3 Hydrogen Spectrum 2.4 Balmer Series 2.5 The Rydberg Formula 3. Bohr’s Theory 3.1 Bohr Model 3.2 Line Spectra 3.3 Multi-electron Atoms 4. Summary CHEMISTRY PAPER No. : 8 (PHYSICAL SPECTROSCOPY) MODULE No. : 7 (BOHR’S THEORY AND SPECTRA OF HYDROGEN AND HYDROGEN-LIKE IONS) ____________________________________________________________________________________________________ 1. Learning Outcomes After studying this module, you should be able to grasp the important ideas of Bohr’s Theory of the structure of atomic hydrogen. We will first review the experimental observations of the atomic spectrum of hydrogen, which led to the birth of quantum mechanics. 2. What is a Spectrum? 2.1 Introduction In spectroscopy, we are interested in the absorption and emission of radiation by matter and its consequences. A spectrum is the distribution of photon energies coming from a light source: • How many photons of each energy are emitted by the light source? Spectra are observed by passing light through a spectrograph: • Breaks the light into its component wavelengths and spreads them apart (dispersion). • Uses either prisms or diffraction gratings. The absorption and emission of photons are governed by the Bohr condition ΔE = hν. -
Series 1 Atoms and Bohr Model.Pdf
Atoms and the Bohr Model Reading: Gray: (1-1) to (1-7) OGN: (15.1) and (15.4) Outline of First Lecture I. General information about the atom II. How the theory of the atomic structure evolved A. Charge and Mass of the atomic particles 1. Faraday 2. Thomson 3. Millikan B. Rutherford’s Model of the atom Reading: Gray: (1-1) to (1-7) OGN: (15.1) and (15.4) H He Li Be B C N O F Ne Na Mg Al Si P S Cl Ar K Ca Sc Ti V Cr Mn Fe Co Ni Cu Zn Ga Ge As Se Br Kr Rb Sr Y Zr Nb Mo Tc Ru Rh Pd Ag Cd In Sn Sb Te I Xe Cs Ba La Hf Ta W Re Os Ir Pt Au Hg Tl Pb Bi Po At Rn Fr Ra Ac Ce Pr Nd Pm Sm Eu Gd Tb Dy Ho Er Tm Yb Lu Th Pa U Np Pu Am Cm Bk Cf Es Fm Md No Lr Atoms consist of: Mass (a.m.u.) Charge (eu) 6 6 Protons ~1 +1 Neutrons ~1 0 C Electrons 1/1836 -1 12.01 10-5 Å (Nucleus) Electron Cloud 1 Å 1 Å = 10 –10 m Note: Nucleus not drawn to scale! HOWHOW DODO WEWE KNOW:KNOW: Atomic Size? Charge and Mass of an Electron? Charge and Mass of a Proton? Mass Distribution in an Atom? Reading: Gray: (1-1) to (1-7) OGN: (15.1) and (15.4) A Timeline of the Atom 400 BC ..... -
A History of Astronomy, Astrophysics and Cosmology - Malcolm Longair
ASTRONOMY AND ASTROPHYSICS - A History of Astronomy, Astrophysics and Cosmology - Malcolm Longair A HISTORY OF ASTRONOMY, ASTROPHYSICS AND COSMOLOGY Malcolm Longair Cavendish Laboratory, University of Cambridge, JJ Thomson Avenue, Cambridge CB3 0HE Keywords: History, Astronomy, Astrophysics, Cosmology, Telescopes, Astronomical Technology, Electromagnetic Spectrum, Ancient Astronomy, Copernican Revolution, Stars and Stellar Evolution, Interstellar Medium, Galaxies, Clusters of Galaxies, Large- scale Structure of the Universe, Active Galaxies, General Relativity, Black Holes, Classical Cosmology, Cosmological Models, Cosmological Evolution, Origin of Galaxies, Very Early Universe Contents 1. Introduction 2. Prehistoric, Ancient and Mediaeval Astronomy up to the Time of Copernicus 3. The Copernican, Galilean and Newtonian Revolutions 4. From Astronomy to Astrophysics – the Development of Astronomical Techniques in the 19th Century 5. The Classification of the Stars – the Harvard Spectral Sequence 6. Stellar Structure and Evolution to 1939 7. The Galaxy and the Nature of the Spiral Nebulae 8. The Origins of Astrophysical Cosmology – Einstein, Friedman, Hubble, Lemaître, Eddington 9. The Opening Up of the Electromagnetic Spectrum and the New Astronomies 10. Stellar Evolution after 1945 11. The Interstellar Medium 12. Galaxies, Clusters Of Galaxies and the Large Scale Structure of the Universe 13. Active Galaxies, General Relativity and Black Holes 14. Classical Cosmology since 1945 15. The Evolution of Galaxies and Active Galaxies with Cosmic Epoch 16. The Origin of Galaxies and the Large-Scale Structure of The Universe 17. The VeryUNESCO Early Universe – EOLSS Acknowledgements Glossary Bibliography Biographical SketchSAMPLE CHAPTERS Summary This chapter describes the history of the development of astronomy, astrophysics and cosmology from the earliest times to the first decade of the 21st century. -
Arxiv:1512.01765V2 [Physics.Atom-Ph]
August12,2016 1:27 WSPCProceedings-9.75inx6.5in Antognini˙ICOLS˙3 page 1 1 Muonic atoms and the nuclear structure A. Antognini∗ for the CREMA collaboration Institute for Particle Physics, ETH, 8093 Zurich, Switzerland Laboratory for Particle Physics, Paul Scherrer Institute, 5232 Villigen-PSI, Switzerland ∗E-mail: [email protected] High-precision laser spectroscopy of atomic energy levels enables the measurement of nu- clear properties. Sensitivity to these properties is particularly enhanced in muonic atoms which are bound systems of a muon and a nucleus. Exemplary is the measurement of the proton charge radius from muonic hydrogen performed by the CREMA collaboration which resulted in an order of magnitude more precise charge radius as extracted from other methods but at a variance of 7 standard deviations. Here, we summarize the role of muonic atoms for the extraction of nuclear charge radii, we present the status of the so called “proton charge radius puzzle”, and we sketch how muonic atoms can be used to infer also the magnetic nuclear radii, demonstrating again an interesting interplay between atomic and particle/nuclear physics. Keywords: Proton radius; Muon; Laser spectroscopy, Muonic atoms; Charge and mag- netic radii; Hydrogen; Electron-proton scattering; Hyperfine splitting; Nuclear models. 1. What atomic physics can do for nuclear physics The theory of the energy levels for few electrons systems, which is based on bound- state QED, has an exceptional predictive power that can be systematically improved due to the perturbative nature of the theory itself [1, 2]. On the other side, laser spectroscopy yields spacing between energy levels in these atomic systems so pre- cisely, that even tiny effects related with the nuclear structure already influence several significant digits of these measurements. -
Compton Wavelength, Bohr Radius, Balmer's Formula and G-Factors
Compton wavelength, Bohr radius, Balmer's formula and g-factors Raji Heyrovska J. Heyrovský Institute of Physical Chemistry, Academy of Sciences of the Czech Republic, Dolejškova 3, 182 23 Prague 8, Czech Republic. [email protected] Abstract. The Balmer formula for the spectrum of atomic hydrogen is shown to be analogous to that in Compton effect and is written in terms of the difference between the absorbed and emitted wavelengths. The g-factors come into play when the atom is subjected to disturbances (like changes in the magnetic and electric fields), and the electron and proton get displaced from their fixed positions giving rise to Zeeman effect, Stark effect, etc. The Bohr radius (aB) of the ground state of a hydrogen atom, the ionization energy (EH) and the Compton wavelengths, λC,e (= h/mec = 2πre) and λC,p (= h/mpc = 2πrp) of the electron and proton respectively, (see [1] for an introduction and literature), are related by the following equations, 2 EH = (1/2)(hc/λH) = (1/2)(e /κ)/aB (1) 2 2 (λC,e + λC,p) = α2πaB = α λH = α /2RH (2) (λC,e + λC,p) = (λout - λin)C,e + (λout - λin)C,p (3) α = vω/c = (re + rp)/aB = 2πaB/λH (4) aB = (αλH/2π) = c(re + rp)/vω = c(τe + τp) = cτB (5) where λH is the wavelength of the ionizing radiation, κ = 4πεo, εo is 2 the electrical permittivity of vacuum, h (= 2πħ = e /2εoαc) is the 2 Planck constant, ħ (= e /κvω) is the angular momentum of spin, α (= vω/c) is the fine structure constant, vω is the velocity of spin [2], re ( = ħ/mec) and rp ( = ħ/mpc) are the radii of the electron and -
Muonic Hydrogen: All Orders Calculations
Muonic Hydrogen: all orders calculations Paul Indelicato ECT* Workshop on the Proton Radius Puzzle, Trento, October 29-November 2, 2012 Theory • Peter Mohr, National Institute of Standards and Technology, Gaithersburg, Maryland • Paul Indelicato, Laboratoire Kastler Brossel, École Normale Supérieure, CNRS, Université Pierre et Marie Curie, Paris, France and Helmholtz Alliance HA216/ EMMI (Extreme Mater Institute) Trento, October 2012 2 Present status • Published result: – 49 881.88(76)GHz ➙rp= 0.84184(67) fm – CODATA 2006: 0.8768(69) fm (mostly from hydrogen and electron-proton scattering) – Difference: 5 σ • CODATA 2010 (on line since mid-june 2011) – 0.8775 (51) fm – Difference: 6.9 σ – Reasons (P.J. Mohr): • improved hydrogen calculation • new measurement of 1s-3s at LKB (F. Biraben group) • Mainz electron-proton scattering result • The mystery deepens... – Difference on the muonic hydrogen Lamb shift from the two radii: 0.3212 (51 µH) (465 CODATA) meV Trento, October 2012 3 Hydrogen QED corrections QED at order α and α2 Self Energy Vacuum Polarization H-like “One Photon” order α H-like “Two Photon” order α2 = + + +! Z α expansion; replace exact Coulomb propagator by expansion in number of interactions with the nucleus Trento, October 2012 5 Convergence of the Zα expansion Trento, October 2012 6 Two-loop self-energy (1s) V. A. Yerokhin, P. Indelicato, and V. M. Shabaev, Phys. rev. A 71, 040101(R) (2005). Trento, October 2012 7 Two-loop self-energy (1s) V. A. Yerokhin, P. Indelicato, and V. M. Shabaev, Phys. rev. A 71, 040101(R) (2005). V. A. Yerokhin, Physical Review A 80, 040501 (2009) Trento, October 2012 8 Evolution at low-Z All order numerical calculations V. -
Physiker-Entdeckungen Und Erdzeiten Hans Ulrich Stalder 31.1.2019
Physiker-Entdeckungen und Erdzeiten Hans Ulrich Stalder 31.1.2019 Haftungsausschluss / Disclaimer / Hyperlinks Für fehlerhafte Angaben und deren Folgen kann weder eine juristische Verantwortung noch irgendeine Haftung übernommen werden. Änderungen vorbehalten. Ich distanziere mich hiermit ausdrücklich von allen Inhalten aller verlinkten Seiten und mache mir diese Inhalte nicht zu eigen. Erdzeiten Erdzeit beginnt vor x-Millionen Jahren Quartär 2,588 Neogen 23,03 (erste Menschen vor zirka 4 Millionen Jahren) Paläogen 66 Kreide 145 (Dinosaurier) Jura 201,3 Trias 252,2 Perm 298,9 Karbon 358,9 Devon 419,2 Silur 443,4 Ordovizium 485,4 Kambrium 541 Ediacarium 635 Cryogenium 850 Tonium 1000 Stenium 1200 Ectasium 1400 Calymmium 1600 Statherium 1800 Orosirium 2050 Rhyacium 2300 Siderium 2500 Physiker Entdeckungen Jahr 0800 v. Chr.: Den Babyloniern sind Sonnenfinsterniszyklen mit der Sarosperiode (rund 18 Jahre) bekannt. Jahr 0580 v. Chr.: Die Erde wird nach einer Theorie von Anaximander als Kugel beschrieben. Jahr 0550 v. Chr.: Die Entdeckung von ganzzahligen Frequenzverhältnissen bei konsonanten Klängen (Pythagoras in der Schmiede) führt zur ersten überlieferten und zutreffenden quantitativen Beschreibung eines physikalischen Sachverhalts. © Hans Ulrich Stalder, Switzerland Jahr 0500 v. Chr.: Demokrit postuliert, dass die Natur aus Atomen zusammengesetzt sei. Jahr 0450 v. Chr.: Vier-Elemente-Lehre von Empedokles. Jahr 0300 v. Chr.: Euklid begründet anhand der Reflexion die geometrische Optik. Jahr 0265 v. Chr.: Zum ersten Mal wird die Theorie des Heliozentrischen Weltbildes mit geometrischen Berechnungen von Aristarchos von Samos belegt. Jahr 0250 v. Chr.: Archimedes entdeckt das Hebelgesetz und die statische Auftriebskraft in Flüssigkeiten, Archimedisches Prinzip. Jahr 0240 v. Chr.: Eratosthenes bestimmt den Erdumfang mit einer Gradmessung zwischen Alexandria und Syene. -
Excitons in 3D and 2D Systems
Excitons in 3D and 2D systems Electrons and holes in an excited semiconductor create a quasiparticle, named exciton. After separation of centre of gravity and relative orbital motion a series of bound exciton states (n=1,2,3…) are located below the band gap. Solving the Schrödinger equation the binding energy in 3D is R * E X (3D) ,n 1,2,.... n n2 *e4 Where R* is the Rydberg energy by R* 2 2 2 2 with µ* as reduced effective mass. It 32 0 defines a series of exciton states which can be populated. In analogy to the hydrogen problem the respective orbital wave function for n=1 is X 1 r (r) exp( ) n1 3/ 2 a0 a0 2 X 4 0 With exciton Bohr radius a (3D) and r=re-rh is the 3D relative electron-hole 0 *e2 coordinate. In k-Space the wave function represented by 3/ 2 X 8 a0 n1 (k) 2 2 2 (1 a0 k ) The k-space representation is important to estimate the oscillator strength of excitonic processes. For discussion of PL excitation spectra and the bleaching of exciton absorption it is important to consider the influence of unbound electron-hole states above the ionization limit (E>0). It is expressed by the Sommerfeld factor 2 R * /( E ) 3D 3D g CEF | E0 (r 0) 1 exp(2 R * /( Eg ) This equation describes the enhancement of absorption above the band gap due to correlated electron-hole pairs. Since equ. Above diverges for Eg one observes a “tooth-like” absorption line.