The Evolution of Stars

Total Page:16

File Type:pdf, Size:1020Kb

The Evolution of Stars The Evolution of Stars The Evolution of Stars: From Birth to Death By Graham Hill The Evolution of Stars: From Birth to Death By Graham Hill This book first published 2020 Cambridge Scholars Publishing Lady Stephenson Library, Newcastle upon Tyne, NE6 2PA, UK British Library Cataloguing in Publication Data A catalogue record for this book is available from the British Library Copyright © 2020 by Graham Hill All rights for this book reserved. No part of this book may be reproduced, stored in a retrieval system, or transmitted, in any form or by any means, electronic, mechanical, photocopying, recording or otherwise, without the prior permission of the copyright owner. ISBN (10): 1-5275-5052-4 ISBN (13): 978-1-5275-5052-0 To Willem J Luyten who gave me the opportunity to become a professional astronomer and who, each day, demonstrated that age is no barrier to imagination and innovation. And to my wife Joanie, who has been my rock over many years, particularly over this last year. Frontispiece. See Centrefold. The Spirograph Nebula. Credit: NASA and The Hubble Heritage Team/(STScI/AURA) CONTENTS List of Tables ........................................................................................... xii Preface .................................................................................................... xiii Prologue ................................................................................................... xv 1 Background ............................................................................................ 1 1.1 What’s with astronomy? Who cares? 1.2 The nature of astronomy 1.3 The window to the Universe: The electromagnetic spectrum 1.4 Neutrinos 1.5 Gravity waves (GWs) 1.6 Cosmic Rays 1.7 A brief reflection 2 The sky and how we view it ................................................................ 27 2.1 Twinkles 2.2 Attenuation of starlight 2.3 Constellations: Not the only legacy from ancient times 2.4 Telescopes: What does a telescope do? 2.5 Refracting telescopes 2.6 Reflecting telescopes 2.7 The current crop of behemoths 2.8 Interferometers: Getting much more for your bucks 2.9 The astronomer's night-time world 2.10 Detectors: The astronomer's eyes 2.11 Advances in optics 2.12 Beating the atmosphere 2.13 Why are telescopes located in weird places? 2.14 Back to the “weird places” 2.15 Uses of computers in astronomy 2.16 Next steps viii Contents 3 Learning about the Sun ....................................................................... 67 3.1 Early days 3.2 Ancient book burning: The library at Alexandria 3.3 Getting started 3.4 Measuring the distance to the Sun 3.5 The size of the Earth 3.6 Aristotle’s views hold things up 3.7 The Copernicum revolution 3.8 Galileo and the telescope 3.9 Kepler 3.10 Newton 3.11 How far away is the Sun? The solar parallax 3.12 The velocity of light 3.13 The Sun’s size 3.14 Measuring the Sun's mass 3.15 The discovery of Uranus: The power of analysis 3.16 An instrumental interlude: The spectrograph 3.17 Spectral lines in the Sun 3.18 Spectra 3.19 The Doppler shift 4 Our first peek: The Sun as a star ....................................................... 94 4.1 Some solar details 4.2 At the Sun's surface 4.3 The solar atmosphere 4.4 What is the Sun made of? 4.5 The Sun's magnetic field 4.6 The solar cycle 4.7 Sunspots and the weather 4.8 Back to Sunspots 4.9 Solar seismology 5 The solar interior ............................................................................... 115 5.1 Origins 5.2 Hubble’s law and the fifth force of Nature? 5.3 Birth of the Sun 5.4 Sources of solar energy generation 5.5 The need for mathematical modelling: Modelling the Sun The Evolution of Stars: From Birth to Death ix 6 What’s out there? First glimmerings ............................................... 137 6.1 Double or binary stars 6.2 Measuring the distance to the stars: The elusive parallax 6.3 A sidebar: The development of mathematical analysis 6.4 Stellar photometry: Measuring brightness and variability 6.5 Stellar positions and motions 6.6 Brightness and colour 7 Stars are not just points of light ....................................................... 152 7.1 The growth of spectroscopy 7.2 The appearance of spectra: Absorption lines 7.3 Stellar classifications 7.4 The Hertzsprung-Russell diagram 7.5 The effects of gravity seen in spectra 7.6 More binary stars 7.7 An aside: The detection of extrasolar planets 8 Assembling our ingredients .............................................................. 178 8.1 Preamble 8.2 The mass-luminosity relation 8.3 Measuring stellar temperatures 8.4 Stellar size 8.5 Stellar densities 8.6 Variable stars 8.7 Abundances: What are stars made of? 8.8 A summary: Our bits and pieces 9 Snapshots of evolution ....................................................................... 199 9.1 A first look at evolution: Early days 9.2 Clusters of stars 9.3 The concept of zero age 9.4 Extending the distance scale 9.5 Cepheid variables: Stars that pulsate 9.6 RR Lyrae variables: Other stars that pulsate 9.7 A complication: Interstellar reddening or dust 9.8 The spacecraft Hipparcos 10 A pathway to diamonds ................................................................... 220 10.1 Boundaries 10.2 A cosmic jigsaw puzzle 10.3 Stellar nurseries x Contents 10.4 How do we evolve a model star? 10.5 From interstellar gas and dust, to the Sun 10.6 The main sequence Sun 10.7 Off the main sequence 10.8 The helium flash 10.9 Pulsating RR Lyrae stars 10.10 To the asymptotic giant branch 10.11 Smoke rings: The formation of a planetary nebula 10.12 From under the carpet 10.13 The end of the line: The formation of a white dwarf 10.14 Stars less than 0.075 solar masse 10.15 Stars less than 0.7 solar masses 10.16 A summary. What have we got so far 10.17 Complications: Surprise! Surprise! 11 On the fast track to oblivion ........................................................... 252 11.1 Helter skelter 11.2 Back to the story 11.3 The end of the line 11.4 More about supernovae 11.5 Summary 12 Resulting weirdoes, the products of evolution ............................... 266 12.1 Preamble 12.2 White dwarfs 12.3 Neutron stars 12.4 Black Holes 12.5 Brown dwarfs: Little stars that couldn’t 12.6 Missing mass: Yet more of it! 13 Prove it! ............................................................................................ 291 13.1 How do you know you’ve got it right? 13.2 The data 13.3 Obtaining cluster data 13.4 Generating the models 13.5 On the way to evolution: Generating a ZAMS 13.6 How do you match theory with observations? 13.7 The Cepheids 13.8 RR Lyrae stars and the Horizontal Branch 13.9 What can eclipsing binaries tell us? 13.10 White dwarfs The Evolution of Stars: From Birth to Death xi 13.11 Neutron stars and pulsars 13.12 Black holes 13.13 Summing up 14 And so they came, two by two ......................................................... 334 14.1 Binary star evolution: The Roche model 14.2 Modelling a binary system: Getting started 14.3 Detached systems 14.4 Back to detached systems 14.5 Semi-detached systems 14.6 Contact systems (W UMa binaries) 14.7 End-of-life variations 14.8 Detecting neutron stars in orbit 14.9 A brief wrap-up 15 Where is astronomy heading? ........................................................ 355 15.1 Big data 15.2 OGLE 15.3 Gaia 15.4 The behemoths: Ground-based 15.5 Satellite-borne telescopes 15.6 Telescopes: A census 15.7 A fantasy? The Overwhelmingly Large Telescope (OWL) 15.8 Where is astronomy heading? 15.9 My omissions 15.10 Last words Glossary ................................................................................................. 383 Journal Abbreviations .......................................................................... 417 List of Illustrations and Figures .......................................................... 418 LIST OF TABLES Table 3.1. A comparison of planet-Sun distances Table 5.1. The run of temperature, density and mass as a function of radius in the solar interior Table 7.1. A coarse summary of spectral classes Table 8.1. Some comparative mean densities Table 10.1. Mass limits and evolutionary destinations PREFACE “Twinkle, twinkle, little star How I wonder what you are Up above the world so high Like a diamond in the sky Twinkle, twinkle little star How I wonder what you are” This book had its genesis more than sixty years ago when I read W. M. Smart's book “Some Famous Stars”. It was, and still is, a wonderfully informative book on astronomy and was influential in setting me on my path to becoming an astronomer. Now, in my mature years, I've responded to the heeding of my wife who has long urged me to write about astronomy though not in a technical manner for I have authored and co-authored many papers on the subject. Her drive, and that of our children and close friends, was for me to write a popular book about the stars that might interest a public who have long been fascinated by astronomy. This is an interest only whetted further by the flow of results from the Hubble Space Telescope, the huge ten-metre-class ground-based telescopes such as the Keck twins on Mauna Kea, the quartet of eight-metre European telescopes in northern Chile and other more esoteric observatories currently in space. Unlike Smart who wrote about a few specific stars, I have chosen to write the story of the evolution of stars from birth to death, but not just of single stars. About 50% of the stars in the sky come in pairs that are gravitationally linked, just as the Earth and Moon are linked, as is the Earth-Moon system to the Sun. Because of this physical connection between stars, the possibilities involved in their evolution take some curious and very interesting paths, much as in our own lives which are more complex when lived with a partner. Most people know little about those little points of light out there we call the stars.
Recommended publications
  • Seasonal and Spatial Variations in the Attenuation of Light in the North Atlantic Ocean
    JEFFREY H. SMART SEASONAL AND SPATIAL VARIATIONS IN THE ATTENUATION OF LIGHT IN THE NORTH ATLANTIC OCEAN This article examines seasonal and spatial vanatlOns in the average depth profiles of the diffuse attenuation coefficient, Kd, for visible light propagating downward from the ocean surface at wavelengths of 490 and 532 nm. Profiles of the depth of the nth attenuation length are also shown. Spring, summer, and fall data from the northwestern and north central Atlantic Ocean and winter data from the northeastern Atlantic Ocean are studied. Variations in the depth-integrated Kd profiles are important because they are related to the depth penetration achievable by an airborne active optical antisubmarine warfare system. INTRODUCTION Numerous investigators have tried to characterize the the geographic areas and seasons indicated in Table 1 and diffuse attenuation coefficient (hereafter denoted as Kd) Figure 1. Despite the incomplete spatial and temporal for various ocean areas and for the different seasons. Platt coverage across the North Atlantic Ocean, this article and Sathyendranath 1 generated numerical fits to averaged should serve as a useful resource to estimate the optical profiles from coastal and open-ocean regions, and they characteristics in the areas studied. divided the North Atlantic into provinces that extended The purpose of this article is to characterize the sea­ from North America to Europe and over large ranges sonal and spatial variations in diffuse attenuation at 490 in latitude (e.g. , from 10.0° to 37.00 N and from 37.0° to and 532 nm. Because Kd frequently changes with depth, 50.00 N). In addition, numerous papers have attempted profiles of depth versus number of attenuation lengths are to model chlorophyll concentrations (which are closely required to characterize the attenuation of light as it correlated with Kd ) using data on available sunlight as a propagates from the surface downward into the water function of latitude and season, nutrient concentrations, column.
    [Show full text]
  • Reason in Motion
    Student Works 11-9-2018 Reason in Motion Luke Francis Embry-Riddle Aeronautical University, [email protected] Follow this and additional works at: https://commons.erau.edu/student-works Part of the Philosophy of Science Commons, and the The Sun and the Solar System Commons Scholarly Commons Citation Francis, L. (2018). Reason in Motion. , (). Retrieved from https://commons.erau.edu/student-works/82 This Article is brought to you for free and open access by Scholarly Commons. It has been accepted for inclusion in Student Works by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. Reason in Motion Luke Francis∗ Embry Riddle Aeronautical University Prescott, AZ 86301 (Dated: November 9, 2018) This essay will explain the historical models of the solar system, which was the known universe for most of human history. There is far more to each model than simply positioning different celestial bodies at the center of the system, and the stories of the astronomers who derived the controversial theories are not discussed often enough. The creation of these theories is part of a much broader revolution in scientific thought and marked the start of a series of observational discoveries that would change the the philosophy of science for centuries to come. I. STUDY PURPOSE Model. This was also influenced by metaphysical notions of human importance. In other words, man saw himself Although science and history are seen as two very sep- as the most important and the most divinely endowed arate fields of study, they depend greatly on each other.
    [Show full text]
  • Natural and Enhanced Attenuation of Soil and Ground Water At
    LMS/MON/S04243 Office of Legacy Management Natural and Enhanced Attenuation of Soil and Groundwater at Monument Valley, Arizona, and Shiprock, New Mexico, DOE Legacy Waste Sites 2007 Pilot Study Status Report June 2008 U.S. Department OfficeOffice ofof LegacyLegacy ManagementManagement of Energy Work Performed Under DOE Contract No. DE–AM01–07LM00060 for the U.S. Department of Energy Office of Legacy Management. Approved for public release; distribution is unlimited. This page intentionally left blank LMS/MON/S04243 Natural and Enhanced Attenuation of Soil and Groundwater at Monument Valley, Arizona, and Shiprock, New Mexico, DOE Legacy Waste Sites 2007 Pilot Study Status Report June 2008 This page intentionally left blank Contents Acronyms and Abbreviations ....................................................................................................... vii Executive Summary....................................................................................................................... ix 1.0 Introduction......................................................................................................................1–1 2.0 Monument Valley Pilot Studies.......................................................................................2–1 2.1 Source Containment and Removal..........................................................................2–1 2.1.1 Phreatophyte Growth and Total Nitrogen...................................................2–1 2.1.2 Causes and Recourses for Stunted Plant Growth........................................2–5
    [Show full text]
  • 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.
    [Show full text]
  • Atmosphere Observation by the Method of LED Sun Photometry
    Atmosphere Observation by the Method of LED Sun Photometry A Senior Project presented to the Faculty of the Physics Department California Polytechnic State University, San Luis Obispo In Partial Fulfillment of the Requirements of the Degree Bachelor of Science by Gregory Garza April 2013 1 Introduction The focus of this project is centered on the subject of sun photometry. The goal of the experiment was to use a simple self constructed sun photometer to observe how attenuation coefficients change over longer periods of time as well as the determination of the solar extraterrestrial constants for particular wavelengths of light. This was achieved by measuring changes in sun radiance at a particular location for a few hours a day and then use of the Langley extrapolation method on the resulting sun radiance data set. Sun photometry itself is generally involved in the practice of measuring atmospheric aerosols and water vapor. Roughly a century ago, the Smithsonian Institutes Astrophysical Observatory developed a method of measuring solar radiance using spectrometers; however, these were not usable in a simple hand-held setting. In the 1950’s Frederick Volz developed the first hand-held sun photometer, which he improved until coming to the use of silicon photodiodes to produce a photocurrent. These early stages of the development of sun photometry began with the use of silicon photodiodes in conjunction with light filters to measure particular wavelengths of sunlight. However, this method of sun photometry came with cost issues as well as unreliability resulting from degradation and wear on photodiodes. A more cost effective method was devised by amateur scientist Forrest Mims in 1989 that incorporated the use of light emitting diodes, or LEDs, that are responsive only to the light wavelength that they emit.
    [Show full text]
  • Radio Astronomy
    Edition of 2013 HANDBOOK ON RADIO ASTRONOMY International Telecommunication Union Sales and Marketing Division Place des Nations *38650* CH-1211 Geneva 20 Switzerland Fax: +41 22 730 5194 Printed in Switzerland Tel.: +41 22 730 6141 Geneva, 2013 E-mail: [email protected] ISBN: 978-92-61-14481-4 Edition of 2013 Web: www.itu.int/publications Photo credit: ATCA David Smyth HANDBOOK ON RADIO ASTRONOMY Radiocommunication Bureau Handbook on Radio Astronomy Third Edition EDITION OF 2013 RADIOCOMMUNICATION BUREAU Cover photo: Six identical 22-m antennas make up CSIRO's Australia Telescope Compact Array, an earth-rotation synthesis telescope located at the Paul Wild Observatory. Credit: David Smyth. ITU 2013 All rights reserved. No part of this publication may be reproduced, by any means whatsoever, without the prior written permission of ITU. - iii - Introduction to the third edition by the Chairman of ITU-R Working Party 7D (Radio Astronomy) It is an honour and privilege to present the third edition of the Handbook – Radio Astronomy, and I do so with great pleasure. The Handbook is not intended as a source book on radio astronomy, but is concerned principally with those aspects of radio astronomy that are relevant to frequency coordination, that is, the management of radio spectrum usage in order to minimize interference between radiocommunication services. Radio astronomy does not involve the transmission of radiowaves in the frequency bands allocated for its operation, and cannot cause harmful interference to other services. On the other hand, the received cosmic signals are usually extremely weak, and transmissions of other services can interfere with such signals.
    [Show full text]
  • GENERALIZED DEFORMATION-RATES in SECONDARY FLOWS of VISCOELASTIC FLUIDS BETWEEN ROTATING SPHERES Redacted for Privacy Kbstract Approved: M.N.L
    AN ABSTRACT OF THE THESIS OF RONALD NORMAN KNOSHAUG for the MASTER OF ARTS (Name) (Degree) in MATHEMATICS presented on October 10, 1968 (Major) (Date) Title: GENERALIZED DEFORMATION-RATES IN SECONDARY FLOWS OF VISCOELASTIC FLUIDS BETWEEN ROTATING SPHERES Redacted for Privacy kbstract approved: M.N.L. Narasimhan By various experiments, it has been found that the re- sponse of real materials to external forces is, in general, nonlinear in character. In classical continuum mechanics, the use of ordinary measures of strain have forced the constitutive equations to take complex forms and since the orders of these measures are not fixed, many unknown re- sponse coefficients have to be introduced into the consti- tutive equations. In general, there is no basis of choos- ing these coefficients. Seth attempted to resolve this difficulty by introducing generalized measures in continuum mechanics and Narasimhan and Sra extended these measures in such a way as to adequately explain some rheological behav- ior of materials. The constitutive equation of Narasimhan and Sra essentially contains two terms and four rheological constants and, unlike some previous theories, it does not contain any unknown functions of the invariants of kine- matic matrices while at the same time explains many visco- elastic phenomena. In the present investigation, a theorem has been proved establishing certain criteria for fixing the orders of generalized measures suitably so as to predict different types of viscoelastic phenomena, such as dilatancy. We have found during the course of this investigation that the constitutive equation of Narasimhan and Sra does not ade- quately explain such physical phenomena as pseudoplasticity.
    [Show full text]
  • Revolution of Charged Particles in a Central Field of Attraction with Emission of Radiation
    ISSN: 2639-0108 Research Article Advances in Theoretical & Computational Physics Revolution of Charged Particles in a Central Field of Attraction with Emission of Radiation Musa D Abdullahi *Corresponding author Musa D Abdullahi, Department of Electrical and Electronics Engineering, Department of Electrical and Electronics Engineering Kaduna Polytechnic, Kaduna, Nigeria. Submitted: 09 Jan 2020; Accepted: 20 Jan 2020; Published: 01 Feb 2020 Abstract A particle of mass nm, carrying the electronic charge -e, revolves in an orbit through angle ψ at distances nr from a center of force of attraction, with angular momenta nL perpendicular to the orbital plane, where n is an integer greater than 0, m the electronic mass and r1 is the radius of the first circular orbit. The equation of motion of the nth orbit of revolution is derived, revealing that an excited particle revolves in an unclosed elliptic orbit, with emission of radiation at the frequency of revolution, before settling down, after many cycles of ψ, in a stable circular orbit. In unipolar revolution, a radiating particle settles in a circular orbit of radius nr1 round a positively charged nucleus. In bipolar revolution, two radiating particles of the same mass nm and charges e and –e, settle in a circular stable orbit of radius ns1 round a common center of mass, where s1 is the radius of the first orbit. Discrete masses nm and angular momenta nL lead to quantization of the orbits outside Bohr’s quantum mechanics. The frequency of radiation in the bipolar revolution is found to be in conformity with the Balmer-Rydberg formula for the spectral lines of radiation from the atom hydrogen gas.
    [Show full text]
  • Causes of Light Attenuation with Respect to Seagrasses in Upper and Lower Charlotte Harbor
    Causes of Light Attenuation with Respect to Seagrasses in Upper and Lower Charlotte Harbor Final Report Submitted to: Southwest Florida Water Management District Surface Water Improvement and Management Program 7601 U.S. Highway 301 North Tampa, FL 33637 (813) 985-7481 Charlotte Harbor National Estuary Program 4980 Bayline Drive 4th Floor North Fort Myers, Florida 33917 (941) 995-1777 Submitted by: L. Kellie Dixon and Gary J. Kirkpatrick Mote Marine Laboratory 1600 Ken Thompson Parkway Sarasota, FL 34236 (941) 388-4441 September 20, 1999 Mote Marine Laboratory Technical Report No. 650. Please note that pages do not always correspond to those listed in the table of contents. This was caused when the document was converted to a PDF file. Acknowledgments Thanks are due to many, but especially Linda Franklin, Jay Leverone, Tiffany Lutterman, Ari Nissanka, Jon Perry, Joie Simoneaux, Roberta Starke, and David Tomasko. i Table of Contents Acknowledgments.............................................................................................................................i Table of Contents.............................................................................................................................ii List of Tables...................................................................................................................................iv List of Figures...................................................................................................................................v Executive Summary.........................................................................................................................ix
    [Show full text]
  • Mass Attenuation Coefficients of X-Rays in Different Barite Concrete Used in Radiation Protection As Shielding Against Ionizing Radiation
    X congreso Regional Latinoamericano IRPA de Protección y Seguridad Radiológica Radi opro te ce ion: Nuevos Desafíos para un Mundo en Evolución ” Buenos Aires, 12 al 17 de abril, 2015 SOCIEDAD ARGENTINA DE RADIOPROTECCIÓN MASS ATTENUATION COEFFICIENTS OF X-RAYS IN DIFFERENT BARITE CONCRETE USED IN RADIATION PROTECTION AS SHIELDING AGAINST IONIZING RADIATION Almeida Junior, Airton T.1’4’5, Nogueira, M. S.2, Santos, M. A. P3, L. L. Campos 4, Araújo, F. G. S.5, 1 Brazilian Institute for Safety and Health at Work - FUNDACENTRO, Minas Gerais, Brazil 2 Center of Development of Nuclear Technology - CDTN/CNEN, Minas Gerais, Brazil 3 Regional Center for Nuclear Science - CRCN/CNEN, Pernambuco, Brazil 4 Institute of Energy and Nuclear Research - IPEN/CNEN, São Paulo, Brazil 5 Universidade Federal de Ouro Preto - UFOP /REDEMAT, Minas Gerais, Brazil ABSTRACT The attenuation coefficient depends on the incident photon energy and the nature of the materials. In order to minimize exposure to individuals. Barite concrete has been largely used as a shielding material in installations housing gamma radiation sources as well as X-ray generating equipment. This study was conducted to evaluate the efficacy of different mixtures of barite concrete for shielding in diagnostic X-ray rooms. The mass attenuation coefficient (jn/p). The mass attenuation coefficients have been measured by employing the CdTe detector model XR-1OOT. The distance between the source and the exposed surface of all samples was measured by SSD light indicator of machine which was 350 cm. The slope of the linear plot of the intensity transmitted versus specimen thickness would yield the attenuation coefficient.
    [Show full text]
  • Lecture 3. Optical Properties 1
    Lecture 3. Optical properties 1. Attenuation of atmospheric radiation by particulates. Aerosol particles can scatter or/and absorb electromagnetic radiation at different wavelengths. NOTE: aerosol particles also can emit thermal radiation. Scattering is a process, which conserves the total amount of energy, but the direction in which the radiation propagates may be altered. Absorption is a process that removes energy from the electromagnetic radiation field, and converts it to another form. Extinction (or attenuation) is the sum of scattering and absorption, so it represents total effect of medium on radiation passing the medium. In the atmosphere: aerosol particles can scatter and absorb solar and infrared radiation altering air temperature and the rates of photochemical reactions. Key parameters that govern the scattering and absorption of radiation by a particle: i. the wavelength of the incident radiation; ii. the size of the particles, expressed as a dimensional size parameter x: D x (where D is the particle diameter); iii. complex refractive index (or optical constant) of a particle: m = n + i k where n is the real part of the refractive index, k is the imaginary part of the refractive index. Both n and k depend on the wavelength. Important to remember: complex refractive index of a particle is defined by its chemical composition; real part , n , is responsible for scattering. imaginary part, k, is responsible for absorption. If k is equal to 0 at a given wavelength thus a particle does not absorb radiation at this wavelength. Table 3.1 Some refractive indices of atmospheric aerosol substances at = 0.5 m.
    [Show full text]
  • Attenuation by Atmospheric Gases
    Recommendation ITU-R P.676-11 (09/2016) Attenuation by atmospheric gases P Series Radiowave propagation ii Rec. ITU-R P.676-11 Foreword The role of the Radiocommunication Sector is to ensure the rational, equitable, efficient and economical use of the radio- frequency spectrum by all radiocommunication services, including satellite services, and carry out studies without limit of frequency range on the basis of which Recommendations are adopted. The regulatory and policy functions of the Radiocommunication Sector are performed by World and Regional Radiocommunication Conferences and Radiocommunication Assemblies supported by Study Groups. Policy on Intellectual Property Right (IPR) ITU-R policy on IPR is described in the Common Patent Policy for ITU-T/ITU-R/ISO/IEC referenced in Annex 1 of Resolution ITU-R 1. Forms to be used for the submission of patent statements and licensing declarations by patent holders are available from http://www.itu.int/ITU-R/go/patents/en where the Guidelines for Implementation of the Common Patent Policy for ITU-T/ITU-R/ISO/IEC and the ITU-R patent information database can also be found. Series of ITU-R Recommendations (Also available online at http://www.itu.int/publ/R-REC/en) Series Title BO Satellite delivery BR Recording for production, archival and play-out; film for television BS Broadcasting service (sound) BT Broadcasting service (television) F Fixed service M Mobile, radiodetermination, amateur and related satellite services P Radiowave propagation RA Radio astronomy RS Remote sensing systems S Fixed-satellite service SA Space applications and meteorology SF Frequency sharing and coordination between fixed-satellite and fixed service systems SM Spectrum management SNG Satellite news gathering TF Time signals and frequency standards emissions V Vocabulary and related subjects Note: This ITU-R Recommendation was approved in English under the procedure detailed in Resolution ITU-R 1.
    [Show full text]