Chapter 6 Electromagnetic Radiation and the Electronic Structure of the Atom
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7. Gamma and X-Ray Interactions in Matter
Photon interactions in matter Gamma- and X-Ray • Compton effect • Photoelectric effect Interactions in Matter • Pair production • Rayleigh (coherent) scattering Chapter 7 • Photonuclear interactions F.A. Attix, Introduction to Radiological Kinematics Physics and Radiation Dosimetry Interaction cross sections Energy-transfer cross sections Mass attenuation coefficients 1 2 Compton interaction A.H. Compton • Inelastic photon scattering by an electron • Arthur Holly Compton (September 10, 1892 – March 15, 1962) • Main assumption: the electron struck by the • Received Nobel prize in physics 1927 for incoming photon is unbound and stationary his discovery of the Compton effect – The largest contribution from binding is under • Was a key figure in the Manhattan Project, condition of high Z, low energy and creation of first nuclear reactor, which went critical in December 1942 – Under these conditions photoelectric effect is dominant Born and buried in • Consider two aspects: kinematics and cross Wooster, OH http://en.wikipedia.org/wiki/Arthur_Compton sections http://www.findagrave.com/cgi-bin/fg.cgi?page=gr&GRid=22551 3 4 Compton interaction: Kinematics Compton interaction: Kinematics • An earlier theory of -ray scattering by Thomson, based on observations only at low energies, predicted that the scattered photon should always have the same energy as the incident one, regardless of h or • The failure of the Thomson theory to describe high-energy photon scattering necessitated the • Inelastic collision • After the collision the electron departs -
Chapter 3 the Mechanisms of Electromagnetic Emissions
BASICS OF RADIO ASTRONOMY Chapter 3 The Mechanisms of Electromagnetic Emissions Objectives: Upon completion of this chapter, you will be able to describe the difference between thermal and non-thermal radiation and give some examples of each. You will be able to distinguish between thermal and non-thermal radiation curves. You will be able to describe the significance of the 21-cm hydrogen line in radio astronomy. If the material in this chapter is unfamiliar to you, do not be discouraged if you don’t understand everything the first time through. Some of these concepts are a little complicated and few non- scientists have much awareness of them. However, having some familiarity with them will make your radio astronomy activities much more interesting and meaningful. What causes electromagnetic radiation to be emitted at different frequencies? Fortunately for us, these frequency differences, along with a few other properties we can observe, give us a lot of information about the source of the radiation, as well as the media through which it has traveled. Electromagnetic radiation is produced by either thermal mechanisms or non-thermal mechanisms. Examples of thermal radiation include • Continuous spectrum emissions related to the temperature of the object or material. • Specific frequency emissions from neutral hydrogen and other atoms and mol- ecules. Examples of non-thermal mechanisms include • Emissions due to synchrotron radiation. • Amplified emissions due to astrophysical masers. Thermal Radiation Did you know that any object that contains any heat energy at all emits radiation? When you’re camping, if you put a large rock in your campfire for a while, then pull it out, the rock will emit the energy it has absorbed as radiation, which you can feel as heat if you hold your hand a few inches away. -
The Protection of Frequencies for Radio Astronomy 1
JOURNAL OF RESEARCH of the National Bureau of Standards-D. Radio Propagation Vol. 67D, No. 2, March- April 1963 b The Protection of Frequencies for Radio Astronomy 1 R. 1. Smith-Rose President, International Scientific Radio Union (R eceived November 5, 1962) The International T elecommunications Union in its Geneva, 1959 R adio R egulations r recognises the Radio Astronomy Service in t he two following definitions: N o. 74 Radio A st1" onomy: Astronomy based on t he reception of waves of cos mi c origin. No. 75 R adio A st1"onomy Se1"vice: A service involving the use of radio astronomy. This service differs, however, from other r adio services in two important respects. 1. It does not itself originate any radio waves, and therefore causes no interference to any other service. L 2. A large proportion of its activity is conducted by the use of reception techniques which are several orders of magnit ude )]).ore sensitive than those used in other ra dio services. In order to pursue his scientific r esearch successfully, t he radio astronomer seeks pro tection from interference first, in a number of bands of frequencies distributed t hroughout I t he s p ~ct run:; and secondly:. 1~10r e complete and s p ec i~c prote.ction fOl: t he exact frequency bands III whIch natural radIatIOn from, or absorptIOn lD, cosmIc gases IS known or expected to occur. The International R egulations referred to above give an exclusive all ocation to one freq uency band only- the emission line of h ydrogen at 1400 to 1427 Mc/s. -
Photon Cross Sections, Attenuation Coefficients, and Energy Absorption Coefficients from 10 Kev to 100 Gev*
1 of Stanaaros National Bureau Mmin. Bids- r'' Library. Ml gEP 2 5 1969 NSRDS-NBS 29 . A111D1 ^67174 tioton Cross Sections, i NBS Attenuation Coefficients, and & TECH RTC. 1 NATL INST OF STANDARDS _nergy Absorption Coefficients From 10 keV to 100 GeV U.S. DEPARTMENT OF COMMERCE NATIONAL BUREAU OF STANDARDS T X J ". j NATIONAL BUREAU OF STANDARDS 1 The National Bureau of Standards was established by an act of Congress March 3, 1901. Today, in addition to serving as the Nation’s central measurement laboratory, the Bureau is a principal focal point in the Federal Government for assuring maximum application of the physical and engineering sciences to the advancement of technology in industry and commerce. To this end the Bureau conducts research and provides central national services in four broad program areas. These are: (1) basic measurements and standards, (2) materials measurements and standards, (3) technological measurements and standards, and (4) transfer of technology. The Bureau comprises the Institute for Basic Standards, the Institute for Materials Research, the Institute for Applied Technology, the Center for Radiation Research, the Center for Computer Sciences and Technology, and the Office for Information Programs. THE INSTITUTE FOR BASIC STANDARDS provides the central basis within the United States of a complete and consistent system of physical measurement; coordinates that system with measurement systems of other nations; and furnishes essential services leading to accurate and uniform physical measurements throughout the Nation’s scientific community, industry, and com- merce. The Institute consists of an Office of Measurement Services and the following technical divisions: Applied Mathematics—Electricity—Metrology—Mechanics—Heat—Atomic and Molec- ular Physics—Radio Physics -—Radio Engineering -—Time and Frequency -—Astro- physics -—Cryogenics. -
Chapter 30: Quantum Physics ( ) ( )( ( )( ) ( )( ( )( )
Chapter 30: Quantum Physics 9. The tungsten filament in a standard light bulb can be considered a blackbody radiator. Use Wien’s Displacement Law (equation 30-1) to find the peak frequency of the radiation from the tungsten filament. −− 10 1 1 1. (a) Solve Eq. 30-1 fTpeak =×⋅(5.88 10 s K ) for the peak frequency: =×⋅(5.88 1010 s−− 1 K 1 )( 2850 K) =× 1.68 1014 Hz 2. (b) Because the peak frequency is that of infrared electromagnetic radiation, the light bulb radiates more energy in the infrared than the visible part of the spectrum. 10. The image shows two oxygen atoms oscillating back and forth, similar to a mass on a spring. The image also shows the evenly spaced energy levels of the oscillation. Use equation 13-11 to calculate the period of oscillation for the two atoms. Calculate the frequency, using equation 13-1, from the inverse of the period. Multiply the period by Planck’s constant to calculate the spacing of the energy levels. m 1. (a) Set the frequency T = 2π k equal to the inverse of the period: 1 1k 1 1215 N/m f = = = =4.792 × 1013 Hz Tm22ππ1.340× 10−26 kg 2. (b) Multiply the frequency by Planck’s constant: E==×⋅ hf (6.63 10−−34 J s)(4.792 × 1013 Hz) =× 3.18 1020 J 19. The light from a flashlight can be considered as the emission of many photons of the same frequency. The power output is equal to the number of photons emitted per second multiplied by the energy of each photon. -
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 -
Photons Outline
1 Photons Observational Astronomy 2019 Part 1 Prof. S.C. Trager 2 Outline Wavelengths, frequencies, and energies of photons The EM spectrum Fluxes, filters, magnitudes & colors 3 Wavelengths, frequencies, and energies of photons Recall that λν=c, where λ is the wavelength of a photon, ν is its frequency, and c is the speed of light in a vacuum, c=2.997925×1010 cm s–1 The human eye is sensitive to wavelengths from ~3900 Å (1 Å=0.1 nm=10–8 cm=10–10 m) – blue light – to ~7200 Å – red light 4 “Optical” astronomy runs from ~3100 Å (the atmospheric cutoff) to ~1 µm (=1000 nm=10000 Å) Optical astronomers often refer to λ>8000 Å as “near- infrared” (NIR) – because it’s beyond the wavelength sensitivity of most people’s eyes – although NIR typically refers to the wavelength range ~1 µm to ~2.5 µm We’ll come back to this in a minute! 5 The energy of a photon is E=hν, where h=6.626×10–27 erg s is Planck’s constant High-energy (extreme UV, X-ray, γ-ray) astronomers often use eV (electron volt) as an energy unit, where 1 eV=1.602176×10–12 erg 6 Some useful relations: E (erg) 14 ⌫ (Hz) = 1 =2.418 10 E (eV) h (erg s− ) ⇥ ⇥ c hc 1 1 1 λ (A)˚ = = = 12398.4 E− (eV− ) ⌫ ⌫ E (eV) ⇥ Therefore a photon with a wavelength of 10 Å has an energy of ≈1.24 keV 7 If a photon was emitted from a blackbody of temperature T, then the average photon energy is Eav~kT, where k = 1.381×10–16 erg K–1 = 8.617×10–5 eV K–1 is Boltzmann’s constant. -
1 Spectroscopic Study of Unique Line Broadening and Inversion in Low
Spectroscopic study of unique line broadening and inversion in low pressure microwave generated water plasmas R. L. Mills,a) P. C. Ray, R. M. Mayo, M. Nansteel, B. Dhandapani BlackLight Power, Inc., 493 Old Trenton Road, Cranbury, NJ 08512 Jonathan Phillips University of New Mexico, Dept. of Chemical and Nuclear Engineering, 203 Farris Engineering, Albuquerque, NM 87131 It was demonstrated that low pressure (~ 0.2 Torr) water vapor plasmas generated in a 10 mm inner diameter quartz tube with an Evenson microwave cavity show at least two features which are not explained by conventional plasma models. First, significant (> 2.5 Å) hydrogen Balmer α line broadening, of constant width, up to 5 cm from the microwave coupler was recorded. Only hydrogen, and not oxygen, showed significant line broadening. This feature, observed previously in hydrogen-containing mixed gas plasmas generated with high voltage dc and rf discharges was explained by some researchers to result from acceleration of hydrogen ions near the cathode. This explanation cannot apply to the line broadening observed in the (electrodeless) microwave plasmas generated in this work, particularly at distances as great as 5 cm from the microwave coupler. Second, inversion of the line intensities of both the Lyman and Balmer series, again, at distances up to 5 cm from the coupler, were observed. The line inversion suggests the existence of a hitherto unknown source of pumping of the 1 optical power in plasmas. Finally, it is notable that other aspects of the plasma including the OH* rotational temperature and low electron concentrations are quite typical of plasmas of this type. -
The Radio-Frequency Line Spectrum of Atomic Hydrogen and Its Applications in Astronomy
THE RADIO-FREQUENCY LINE SPECTRUM OF ATOMIC HYDROGEN AND ITS APPLICATIONS IN ASTRONOMY J. P. Wild Division of Radiophysics, Commonwealth Scientific and Industrial Research Organization, Australia Received September 8, 1951 ABSTRACT Formulae are obtained for the frequencies, transition probabilities, and natural widths of the dis- crete lines of atomic hydrogen that fall within the radio spectrum. Such lines are due to transitions within either the fine structure or the hyperfine structure of the energy levels. The conditions necessary for the formation of observable emission and absorption lines are examined. Thence an inquiry is made into which of the hydrogen lines are likely to be observable from astronomi- cal systems. It is found that the sun may give a detectable absorption line at about 10,000 Mc/sec, corre- 2 2 sponding to the 2 Si/2-2 P3/2 fine-structure transition, but that other solar fines are not likely to be observable. From the interstellar gas, the emission line already observed (i.e., the 1420 Mc/sec hyper- fine-structure line) is probably the only detectable hydrogen line. The importance of this fine in the study of the interstellar gas is discussed. Some general conclusions are drawn from the preliminary evidence regarding the motion and kinetic temperature of the regions of un-ionized hydrogen. The ratio data are used to obtain a measure of the product of “galactic thickness” and average hydrogen concentration. I. INTRODUCTION The first astronomical observation of a spectral line in the radio-frequency band has recently been announced by Ewen and Purcell1 and has had independent confirmation by two other groups of workers.2,3 The observed line is an emission line of frequency 1420 Mc/sec due to the transition between the hyperfine-s truc ture substates in the ground state of atomic hydrogen. -
Spectra of Photoionized Regions 1. Introduction
Spectra of Photoionized Regions Friday, January 21, 2011 CONTENTS: 1. Introduction 2. Recombination Processes A. Overview B. Level networks C. Free-bound continuum D. Two-photon continuum E. Collisions 3. Additional Processes A. Lyman-α emission B. Helium processes C. Resonance fluorescence 4. Diagnostics A. Temperature B. Density C. Composition D. Star formation rates 1. Introduction Our next task is to consider the emitted spectrum from an H II region. This is one of the most important subjects observationally since spectroscopy provides our principal set of diagnostics on the physics occurring in the region. This material is (mostly) covered in Chapters 4 and 5 of Osterbrock & Ferland (on which most of these notes are based). The sources of emission we will consider fall into two categories: Cooling: Infrared fine structure lines Optical forbidden lines Free-free continuum Recombination: Free-bound continuum Recombination lines Two-photon continuua 1 Generally, the forbidden lines (optical or IR) come from metals, whereas the recombination features are proportional to abundance and arise mainly from H and He. Since the cooling radiation has already been discussed, we will focus on recombination and then proceed to diagnostics. 2. Recombination Processes A. OVERVIEW We first consider the case of recombination of hydrogen at very low densities where the collision rates are small, i.e. any hydrogen atom that forms can decay radiatively before any collision. Later on we will introduce collisions between particles (electrons, protons) with excited atoms. The recombination process at low density begins with a radiative recombination, H+ + e− → H0(nl) + γ , which populates an excited state of the hydrogen atom. -
Ionizing Photon Production from Massive Stars
Ionizing Photon Production from Massive Stars Michael W. Topping CASA, Department of Astrophysical & Planetary Sciences, University of Colorado, Boulder, CO 80309 [email protected] ABSTRACT Ionizing photons are important ingredients in our understanding of stellar and interstellar processes, but modeling their properties can be difficult. This paper examines methods of modeling Lyman Continuum (LyC) photon production us- ing stellar evolutionary tracks coupled to a grid of model atmospheres. In the past, many stellar models have not been self-consistent and have not been able to accurately reproduce stellar population spectra and ionizing photon luminosities. We examine new models of rotating stars at both solar and sub-solar metallicity and show that they increase accuracy of ionizing photon production and satisfy self-consistency relationships. Thesis Advisor: Dr. Michael Shull | Department of Astrophysical and Planetary Sciences Thesis Committee: Dr. John Stocke | Department of Astrophysical and Planetary Sciences Dr. William Ford | Department of Physics Dr. Emily Levesque | Department of Astrophysical and Planetary Sciences Defense Date: March 17, 2014 { 2 { Contents 1 INTRODUCTION 3 1.1 Background . .4 1.1.1 Evolutionary Tracks . .4 1.1.2 Model Atmospheres . .5 2 METHODS 6 2.1 EVOLUTIONARY TRACKS . .7 2.1.1 Old Non-Rotating Tracks (Schaller 1992) . .8 2.1.2 New Non-Rotating Tracks . .8 2.1.3 New Rotating Tracks . .8 2.2 Model Atmospheres . 12 2.2.1 Program Setup . 12 2.2.2 Initial Parameter Files . 12 2.2.3 Model Atmosphere Calculation . 13 2.2.4 Defining the Grid . 15 2.3 Putting It All Together . 15 3 RESULTS 20 3.1 Lifetime Integrated H I Photon Luminosities . -
Hydrogen Line Project Documentation
Welcome to . The Astronomy Zone! In Which Two D&D Nerds Build a Hydrogen Line Radio Telescope Contents: Moonlighting: Overview 2 Petals to the Metal: Horn Antenna Design Analysis 6 The Crystal Kingdom: SDR, Amplification, and Filtering Setup 11 The Eleventh Hour: Finding the Signal in the Noise with GnuRadio 16 The Stolen Century: Data Collection and Analysis 23 Story and Song: Conclusion 32 Here There Be Gerblins: References 34 Moonlighting: Overview Introduction The exact phrases expressing the excitement that started this project are perhaps not appropriate for general audiences. One of us had successfully used their software defined radio to receive images from orbiting NOAA weather satellites, and was looking for a fun challenge. After wandering through the depths of the radio related internet, the Open Source Radio Telescope website revealed images of a device made of lumber, foam insulation paneling, and fairly standard radio equipment. It was a device designed to investigate the structure and motion of clouds of hydrogen gas across the galaxy, the galaxy. Was it really possible? Another link led to the DSPIRA program, using a very similar telescope as part of an NSF program for teachers. It was real! Just one problem: woefully insufficient background in radio astronomy, spectrometry, digital signal processing, or the necessary software. Who cares though, learning by doing is the best way to learn. No sleep was had that night due to excitement and wondering if this could be pulled off in summer. This was too good and too hard not to be shared though, so a late night inquiry was made to a local space-loving physics major and Dungeon Master extraordinaire, and so here we are.