THREE MAIN LIGHT MATTER INTERRACTION
|
|
- Amelia Woods
- 5 years ago
- Views:
Transcription
1 Chapters: 3and 4
2 THREE MAIN LIGHT MATTER INTERRACTION Absorption: converts radiative energy into internal energy Emission: converts internal energy into radiative energy Scattering; Radiative energy is first absorbed and then radiated.
3 Coherent scattering SCATTERING IN DIFFERENT MEDIA Scattering in which radiated wave has a definite phase shift with respect to the incident wave Observed when light is scattered by induced dipoles in a dielectric Incoherent scattering No permanent definite phase relationship between radiated and incident waves and with in the individual scatterred fields. Observed when light is scattered by air or density fluctuations in an ocean.
4 SCATTERING IN DIFFERENT MEDIA Independent scattering Scattering in which radiated field from one scatterer doesnot interract with radiated field from a neighbour scatterer. Average spacing between scatterers should be several times their diameters. Example:Rayleigh scattering.
5 SCATTERING IN DIFFERENT MEDIA Conservative scattering Scattering process in which there is negligible absorption of incident field in the medium Non conservative scattering Scattering process involving relatively much absorption of incident energy in the medium.
6 SCATTERING IN DIFFERENT MEDIA Elastic scattering No exchange of internal energy of the medium with the radiated field No change of frequency of incident wave upon scattering Inelastic scattering Involves exchange of internal energy of the medium with that of the radiated field.
7 SCATTERING IN DIFFERENT MEDIA Optically thin medium: is a medium with well separated particles that when each receives direct radiation,the diffuse radiation from all parts of the medium is negligible compared with direct radiation. Optically thick media This is a medium with a large number of scatteres that the multiply scattered diffuse radiation is more compared with direct radiation. Common to planetary media.
8 RESONANCE SCATTERING If the driving frequency is very close to the natural frequency. The scattering cross section for a damped simple oscillator becomes σ n res = e ۲ ٤m e ε o cπ [ γ/٤π v o v ۲ γ /٤π ۲ ] where: v is driving frequency v o - is natural frequency of oscillator γ is damping rate
9 RAYLEIGH SCATTERING This occurs when driving frequency is less than the natural frequency of the oscillator. The cross section is given as: σ n ray = ۱ ٦π ω c ٤ e ۲ m e ε o ω o ۲ ۲
10 SOURCES OF LINE BROADENING
11 NATURAL BROADENING This occurs when an isolated molecule is irradiated by an electroctromagnetic wave and the dampening of absorption line produced is solely by the natural life time of excited quantum level. Line width of the profile is given as : α= ۱ ۲πt r, t r is natural life time of upper level
12 PRESSURE BROADENING This is due to collisions between molecules that shortens the natural lifetime and broadens the line. Depends on number density and temperature. The broadened width is; α L =α L STP n T n L T o n L - loschmidt number at STP T o is standard temp
13 DOPPLER BROADENING Is as a result of random thermal motion of atoms. The cross section is given as: Doppler width is given by: α D = ν o V o, c where : V o is mean speed of molecules c is speed of light ν o is frequency of molecules.
14 VOIGT PROFILE Is a profile representing combined effects of both lorentz and doppler broadening. Damping ratio: a= α L α D a ۰ shows; doppler result in line core Lorentz like behaviour in the wings a ۱; resembles lorentz for all frequencies
15 COMPARISON OF LINE SHAPES
16 SCATTERING PHASE FUNCTION It is nomalised angular scattering x- section: p cosθ = nσ n cosθ sr ۱ d ωσ n cosθ n ٤π The normalisation is ٤π dw p cosθ ٤π ۲π = ۰ Θ is scattering angle π dφ ۰ dθ sin θ p θ ', φ'; θ. φ ٤π =۱
17 SCATTERING PHASE FUNCTION Rayleigh scattering phase function is : P ray Θ = ۳ ٤ ۱ cos۲ Θ Θ is scattering angle
18 ABSORPTION
19 ABSORPTION Energy selectivity is its outstanding characteristic. Energy attenuation due to absorption is dominant in near infrared and thermal infrared spectral ranges. Absobed radiative enegy in these ranges causes: Excitation of lattice vibrations,molecular vibrational states,and intermolecular vibrations. Absorbed radiative energy in UV and shorter wavelength leads to: Photodissociation,photoionisation
20 ABSORPTION Absorption in solids Conductors have a small gap between the energy bands and are higly absorbing and reflecting in visible and IR. Insulators have a bigger energy gap between the bands,so they are absorbing in UV Insulators are more or less transparent in visible and IR.
21 ABSORPTION Color & brightness of objects Selective absorption is responsible nearlly for all color of objects in the environment An exception rule to this is Rayleigh scattering
22 RADIATION LAWS
23 RADIATION LAWS Planck spectral distribution law is : F BB ν = m ۲ r ۲πhν ۳ c ۲ [exp hν/k B T ۱] Where: h is planck's constant m r - real part of refractive index k B - Boltzmann constant
24 RADIATION LAWS Approximations to F v BB are: ۱. Wiens limit :hv /k B T >> ۱ F BB v m ۲ r c ۲ ۲π hv۳ e hv /k BT ۲. Rayleigh-Jeans limit: hv / k B T << ۱ F v BB ۲πv۲ m r k B T c ۲
25 RADIATION LAWS Wien s displacement law: λ m T =۲,۸۹۷.۸µ mk λ m is wavelength at maximum radiation T is absolute temperature Stefan-Boltzmann law: F v BB =σt ٤ σ is stefan-boltzmann constant T is temperature of the body
Radiation in the Earth's Atmosphere. Part 1: Absorption and Emission by Atmospheric Gases
Radiation in the Earth's Atmosphere Part 1: Absorption and Emission by Atmospheric Gases Electromagnetic Waves Electromagnetic waves are transversal. Electric and magnetic fields are perpendicular. In
More informationLecture 10. Lidar Effective Cross-Section vs. Convolution
Lecture 10. Lidar Effective Cross-Section vs. Convolution q Introduction q Convolution in Lineshape Determination -- Voigt Lineshape (Lorentzian Gaussian) q Effective Cross Section for Single Isotope --
More informationIf light travels past a system faster than the time scale for which the system evolves then t I ν = 0 and we have then
6 LECTURE 2 Equation of Radiative Transfer Condition that I ν is constant along rays means that di ν /dt = 0 = t I ν + ck I ν, (29) where ck = di ν /ds is the ray-path derivative. This is equation is the
More informationChemistry 795T. Lecture 7. Electromagnetic Spectrum Black body Radiation. NC State University
Chemistry 795T Lecture 7 Electromagnetic Spectrum Black body Radiation NC State University Black body Radiation An ideal emitter of radiation is called a black body. Observation: that peak of the energy
More informationChemistry 795T. Black body Radiation. The wavelength and the frequency. The electromagnetic spectrum. Lecture 7
Chemistry 795T Lecture 7 Electromagnetic Spectrum Black body Radiation NC State University Black body Radiation An ideal emitter of radiation is called a black body. Observation: that peak of the energy
More informationPreface to the Second Edition. Preface to the First Edition
Contents Preface to the Second Edition Preface to the First Edition iii v 1 Introduction 1 1.1 Relevance for Climate and Weather........... 1 1.1.1 Solar Radiation.................. 2 1.1.2 Thermal Infrared
More informationWhat is it good for? RT is a key part of remote sensing and climate modeling.
Read Bohren and Clothiaux Ch.; Ch 4.-4. Thomas and Stamnes, Ch..-.6; 4.3.-4.3. Radiative Transfer Applications What is it good for? RT is a key part of remote sensing and climate modeling. Remote sensing:
More informationLecture 4* Inherent optical properties, IOP Theory. Loss due to absorption. IOP Theory 12/2/2008
Lecture 4* Inherent optical properties, part I IOP Theory What properties of a medium affect the radiance field as it propagate through it? 1. Sinks of photons (absorbers) 2. Sources of photons (internal
More informationLecture 2 Blackbody radiation
Lecture 2 Blackbody radiation Absorption and emission of radiation What is the blackbody spectrum? Properties of the blackbody spectrum Classical approach to the problem Plancks suggestion energy quantisation
More informationDescription of radiation field
Description of radiation field Qualitatively, we know that characterization should involve energy/time frequency all functions of x,t. direction We also now that radiation is not altered by passing through
More informationProperties of Electromagnetic Radiation Chapter 5. What is light? What is a wave? Radiation carries information
Concepts: Properties of Electromagnetic Radiation Chapter 5 Electromagnetic waves Types of spectra Temperature Blackbody radiation Dual nature of radiation Atomic structure Interaction of light and matter
More informationGoal: The theory behind the electromagnetic radiation in remote sensing. 2.1 Maxwell Equations and Electromagnetic Waves
Chapter 2 Electromagnetic Radiation Goal: The theory behind the electromagnetic radiation in remote sensing. 2.1 Maxwell Equations and Electromagnetic Waves Electromagnetic waves do not need a medium to
More informationRadiation Processes. Black Body Radiation. Heino Falcke Radboud Universiteit Nijmegen. Contents:
Radiation Processes Black Body Radiation Heino Falcke Radboud Universiteit Nijmegen Contents: Planck Spectrum Kirchoff & Stefan-Boltzmann Rayleigh-Jeans & Wien Einstein Coefficients Literature: Based heavily
More informationModel Answer (Paper code: AR-7112) M. Sc. (Physics) IV Semester Paper I: Laser Physics and Spectroscopy
Model Answer (Paper code: AR-7112) M. Sc. (Physics) IV Semester Paper I: Laser Physics and Spectroscopy Section I Q1. Answer (i) (b) (ii) (d) (iii) (c) (iv) (c) (v) (a) (vi) (b) (vii) (b) (viii) (a) (ix)
More informationChemistry 431. Lecture 1. Introduction Statistical Averaging Electromagnetic Spectrum Black body Radiation. NC State University
Chemistry 431 Lecture 1 Introduction Statistical Averaging Electromagnetic Spectrum Black body Radiation NC State University Overview Quantum Mechanics Failure of classical physics Wave equation Rotational,
More informationMolecular spectroscopy
Molecular spectroscopy Origin of spectral lines = absorption, emission and scattering of a photon when the energy of a molecule changes: rad( ) M M * rad( ' ) ' v' 0 0 absorption( ) emission ( ) scattering
More informationME 476 Solar Energy UNIT TWO THERMAL RADIATION
ME 476 Solar Energy UNIT TWO THERMAL RADIATION Unit Outline 2 Electromagnetic radiation Thermal radiation Blackbody radiation Radiation emitted from a real surface Irradiance Kirchhoff s Law Diffuse and
More informationRadiation in the atmosphere
Radiation in the atmosphere Flux and intensity Blackbody radiation in a nutshell Solar constant Interaction of radiation with matter Absorption of solar radiation Scattering Radiative transfer Irradiance
More informationSkoog Chapter 6 Introduction to Spectrometric Methods
Skoog Chapter 6 Introduction to Spectrometric Methods General Properties of Electromagnetic Radiation (EM) Wave Properties of EM Quantum Mechanical Properties of EM Quantitative Aspects of Spectrochemical
More informationAdvanced Heat and Mass Transfer by Amir Faghri, Yuwen Zhang, and John R. Howell
Advanced Heat and Mass Transfer by Amir Faghri, Yuwen Zhang, and John R. Howell 9.2 The Blackbody as the Ideal Radiator A material that absorbs 100 percent of the energy incident on it from all directions
More informationInteraction of Molecules with Radiation
3 Interaction of Molecules with Radiation Atoms and molecules can exist in many states that are different with respect to the electron configuration, angular momentum, parity, and energy. Transitions between
More informationLaser Beam Interactions with Solids In absorbing materials photons deposit energy hc λ. h λ. p =
Laser Beam Interactions with Solids In absorbing materials photons deposit energy E = hv = hc λ where h = Plank's constant = 6.63 x 10-34 J s c = speed of light Also photons also transfer momentum p p
More informationATMOS 5140 Lecture 7 Chapter 6
ATMOS 5140 Lecture 7 Chapter 6 Thermal Emission Blackbody Radiation Planck s Function Wien s Displacement Law Stefan-Bolzmann Law Emissivity Greybody Approximation Kirchhoff s Law Brightness Temperature
More informationNumerical Heat and Mass Transfer
Master Degree in Mechanical Engineering Numerical Heat and Mass Transfer 11-Radiative Heat Transfer Fausto Arpino f.arpino@unicas.it Nature of Thermal Radiation ü Thermal radiation refers to radiation
More informationChapter 13. Phys 322 Lecture 34. Modern optics
Chapter 13 Phys 3 Lecture 34 Modern optics Blackbodies and Lasers* Blackbodies Stimulated Emission Gain and Inversion The Laser Four-level System Threshold Some lasers Pump Fast decay Laser Fast decay
More informationCHEM6416 Theory of Molecular Spectroscopy 2013Jan Spectroscopy frequency dependence of the interaction of light with matter
CHEM6416 Theory of Molecular Spectroscopy 2013Jan22 1 1. Spectroscopy frequency dependence of the interaction of light with matter 1.1. Absorption (excitation), emission, diffraction, scattering, refraction
More informationHeriot-Watt University
Heriot-Watt University Distinctly Global www.hw.ac.uk Thermodynamics By Peter Cumber Prerequisites Interest in thermodynamics Some ability in calculus (multiple integrals) Good understanding of conduction
More informationAn Introduction to Diffraction and Scattering. School of Chemistry The University of Sydney
An Introduction to Diffraction and Scattering Brendan J. Kennedy School of Chemistry The University of Sydney 1) Strong forces 2) Weak forces Types of Forces 3) Electromagnetic forces 4) Gravity Types
More informationChemistry Instrumental Analysis Lecture 2. Chem 4631
Chemistry 4631 Instrumental Analysis Lecture 2 Electromagnetic Radiation Can be described by means of a classical sinusoidal wave model. Oscillating electric and magnetic field. (Wave model) wavelength,
More informationPhysical Basics of Remote-Sensing with Satellites
- Physical Basics of Remote-Sensing with Satellites Dr. K. Dieter Klaes EUMETSAT Meteorological Division Am Kavalleriesand 31 D-64295 Darmstadt dieter.klaes@eumetsat.int Slide: 1 EUM/MET/VWG/09/0162 MET/DK
More information1. The most important aspects of the quantum theory.
Lecture 5. Radiation and energy. Objectives: 1. The most important aspects of the quantum theory: atom, subatomic particles, atomic number, mass number, atomic mass, isotopes, simplified atomic diagrams,
More informationLecture 3: Optical Properties of Insulators, Semiconductors, and Metals. 5 nm
Metals Lecture 3: Optical Properties of Insulators, Semiconductors, and Metals 5 nm Course Info Next Week (Sept. 5 and 7) no classes First H/W is due Sept. 1 The Previous Lecture Origin frequency dependence
More informationAbsorption Line Physics
Topics: 1. Absorption line shapes 2. Absorption line strength 3. Line-by-line models Absorption Line Physics Week 4: September 17-21 Reading: Liou 1.3, 4.2.3; Thomas 3.3,4.4,4.5 Absorption Line Shapes
More informationThe Black Body Radiation
The Black Body Radiation = Chapter 4 of Kittel and Kroemer The Planck distribution Derivation Black Body Radiation Cosmic Microwave Background The genius of Max Planck Other derivations Stefan Boltzmann
More informationBlackbody radiation. Main Laws. Brightness temperature. 1. Concepts of a blackbody and thermodynamical equilibrium.
Lecture 4 lackbody radiation. Main Laws. rightness temperature. Objectives: 1. Concepts of a blackbody, thermodynamical equilibrium, and local thermodynamical equilibrium.. Main laws: lackbody emission:
More informationAbsorption and scattering
Absorption and scattering When a beam of radiation goes through the atmosphere, it encounters gas molecules, aerosols, cloud droplets, and ice crystals. These objects perturb the radiation field. Part
More informationInteraction X-rays - Matter
Interaction X-rays - Matter Pair production hν > M ev Photoelectric absorption hν MATTER hν Transmission X-rays hν' < hν Scattering hν Decay processes hν f Compton Thomson Fluorescence Auger electrons
More informationLecture 6 - spectroscopy
Lecture 6 - spectroscopy 1 Light Electromagnetic radiation can be thought of as either a wave or as a particle (particle/wave duality). For scattering of light by particles, air, and surfaces, wave theory
More informationQuantum Mechanics (made fun and easy)
Lecture 7 Quantum Mechanics (made fun and easy) Why the world needs quantum mechanics Why the world needs quantum mechanics Why the world needs quantum mechanics Why the world needs quantum mechanics Why
More informationMonday 9 September, :30-11:30 Class#03
Monday 9 September, 2013 10:30-11:30 Class#03 Topics for the hour Solar zenith angle & relationship to albedo Blackbody spectra Stefan-Boltzman Relationship Layer model of atmosphere OLR, Outgoing longwave
More informationQuantum Electronics/Laser Physics Chapter 4 Line Shapes and Line Widths
Quantum Electronics/Laser Physics Chapter 4 Line Shapes and Line Widths 4.1 The Natural Line Shape 4.2 Collisional Broadening 4.3 Doppler Broadening 4.4 Einstein Treatment of Stimulated Processes Width
More informationSpectrum of Radiation. Importance of Radiation Transfer. Radiation Intensity and Wavelength. Lecture 3: Atmospheric Radiative Transfer and Climate
Lecture 3: Atmospheric Radiative Transfer and Climate Radiation Intensity and Wavelength frequency Planck s constant Solar and infrared radiation selective absorption and emission Selective absorption
More informationManuel Gonzalez (IRAM) September 14 th Radiative transfer basics
Manuel Gonzalez (IRAM) September 14 th 2013 Radiative transfer basics What is radiation? Introduction Introduction In Astrophysics radiation from the sources can give us very important information: - Spatial
More informationLecture 3: Atmospheric Radiative Transfer and Climate
Lecture 3: Atmospheric Radiative Transfer and Climate Solar and infrared radiation selective absorption and emission Selective absorption and emission Cloud and radiation Radiative-convective equilibrium
More informationLecture 06. Fundamentals of Lidar Remote Sensing (4) Physical Processes in Lidar
Lecture 06. Fundamentals of Lidar Remote Sensing (4) Physical Processes in Lidar Physical processes in lidar (continued) Doppler effect (Doppler shift and broadening) Boltzmann distribution Reflection
More informationChapter 3 Energy Balance and Temperature. Astro 9601
Chapter 3 Energy Balance and Temperature Astro 9601 1 Topics to be covered Energy Balance and Temperature (3.1) - All Conduction (3..1), Radiation (3.. and 3...1) Convection (3..3), Hydrostatic Equilibrium
More informationThermal Radiation By: Prof. K M Joshi
Thermal Radiation By: Prof. K M Joshi Radiation originate due to emission of matter and its subsequent transports does not required any matter / medium. Que: Then what is the nature of this transport???
More informationLasers PH 645/ OSE 645/ EE 613 Summer 2010 Section 1: T/Th 2:45-4:45 PM Engineering Building 240
Lasers PH 645/ OSE 645/ EE 613 Summer 2010 Section 1: T/Th 2:45-4:45 PM Engineering Building 240 John D. Williams, Ph.D. Department of Electrical and Computer Engineering 406 Optics Building - UAHuntsville,
More information24/ Rayleigh and Raman scattering. Stokes and anti-stokes lines. Rotational Raman spectroscopy. Polarizability ellipsoid. Selection rules.
Subject Chemistry Paper No and Title Module No and Title Module Tag 8/ Physical Spectroscopy 24/ Rayleigh and Raman scattering. Stokes and anti-stokes lines. Rotational Raman spectroscopy. Polarizability
More informationLecture 2: principles of electromagnetic radiation
Remote sensing for agricultural applications: principles and methods Lecture 2: principles of electromagnetic radiation Instructed by Prof. Tao Cheng Nanjing Agricultural University March Crop 11, Circles
More informationLecture 05. Fundamentals of Lidar Remote Sensing (3)
Lecture 05. Fundamentals of Lidar Remote Sensing (3) Physical Processes in Lidar Overview of physical processes in lidar Light transmission through the atmosphere Light interaction with objects Elastic
More information= (fundamental constants c 0, h, k ). (1) k
Introductory Physics Laboratory, Faculty of Physics and Geosciences, University of Leipzig W 12e Radiation Thermometers Tasks 1 Measure the black temperature T s of a glowing resistance wire at eight different
More informationThe Nature of Light I: Electromagnetic Waves Spectra Kirchoff s Laws Temperature Blackbody radiation
The Nature of Light I: Electromagnetic Waves Spectra Kirchoff s Laws Temperature Blackbody radiation Electromagnetic Radiation (How we get most of our information about the cosmos) Examples of electromagnetic
More informationIntroduction to Modern Physics NE 131 Physics for Nanotechnology Engineering
Introduction to Modern Physics NE 131 Physics for Nanotechnology Engineering Dr. Jamie Sanchez-Fortún Stoker Department of Physics, University of Waterloo Fall 2005 1 Introduction to Modern Physics 1.1
More informationChapter 3 Energy Balance and Temperature. Topics to be covered
Chapter 3 Energy Balance and Temperature Astro 9601 1 Topics to be covered Energy Balance and Temperature (3.1) - All Conduction (3..1), Radiation (3.. and31) 3...1) Convection (3..3), Hydrostatic Equilibrium
More informationLaserphysik. Prof. Yong Lei & Dr. Yang Xu. Fachgebiet Angewandte Nanophysik, Institut für Physik
Laserphysik Prof. Yong Lei & Dr. Yang Xu Fachgebiet Angewandte Nanophysik, Institut für Physik Contact: yong.lei@tu-ilmenau.de; yang.xu@tu-ilmenau.de Office: Heisenbergbau V 202, Unterpörlitzer Straße
More informationWavelength λ Velocity v. Electric Field Strength Amplitude A. Time t or Distance x time for 1 λ to pass fixed point. # of λ passing per s ν= 1 p
Introduction to Spectroscopy (Chapter 6) Electromagnetic radiation (wave) description: Wavelength λ Velocity v Electric Field Strength 0 Amplitude A Time t or Distance x Period p Frequency ν time for 1
More informationLecture 2 Global and Zonal-mean Energy Balance
Lecture 2 Global and Zonal-mean Energy Balance A zero-dimensional view of the planet s energy balance RADIATIVE BALANCE Roughly 70% of the radiation received from the Sun at the top of Earth s atmosphere
More informationQM all started with - - The Spectrum of Blackbody Radiation
QM all started with - - The Spectrum of Blackbody Radiation Thermal Radiation: Any object, not at zero temperature, emits electromagnetic called thermal. When we measure the intensity of a real object,
More informationThe Light of Your Life. We can see the universe because atoms emit photons
The Light of Your Life We can see the universe because atoms emit photons Astronomy is an observational science Our messengers are Light (electromagnetic waves) Gravitational waves Cosmic rays (particles)
More informationSpectral Resolution. Spectral resolution is a measure of the ability to separate nearby features in wavelength space.
Spectral Resolution Spectral resolution is a measure of the ability to separate nearby features in wavelength space. R, minimum wavelength separation of two resolved features. Delta lambda often set to
More informationLecture # 04 January 27, 2010, Wednesday Energy & Radiation
Lecture # 04 January 27, 2010, Wednesday Energy & Radiation Kinds of energy Energy transfer mechanisms Radiation: electromagnetic spectrum, properties & principles Solar constant Atmospheric influence
More information3. Stellar Atmospheres: Opacities
3. Stellar Atmospheres: Opacities 3.1. Continuum opacity The removal of energy from a beam of photons as it passes through matter is governed by o line absorption (bound-bound) o photoelectric absorption
More informationNotes on x-ray scattering - M. Le Tacon, B. Keimer (06/2015)
Notes on x-ray scattering - M. Le Tacon, B. Keimer (06/2015) Interaction of x-ray with matter: - Photoelectric absorption - Elastic (coherent) scattering (Thomson Scattering) - Inelastic (incoherent) scattering
More information2. Energy Balance. 1. All substances radiate unless their temperature is at absolute zero (0 K). Gases radiate at specific frequencies, while solids
I. Radiation 2. Energy Balance 1. All substances radiate unless their temperature is at absolute zero (0 K). Gases radiate at specific frequencies, while solids radiate at many Click frequencies, to edit
More informationINTRODUCTION Radiation differs from conduction and convection in that it does not require the presence of a material medium to take place.
RADIATION INTRODUCTION Radiation differs from conduction and convection in that it does not require the presence of a material medium to take place. Radiation: The energy emitted by matter in the form
More informationWith certain caveats (described later) an object absorbs as effectively as it emits
Figure 1: A blackbody defined by a cavity where emission and absorption are in equilibrium so as to maintain a constant temperature Blackbody radiation The basic principles of thermal emission are as follows:
More informationClass 11: Thermal radiation
Class : Thermal radiation By analyzing the results from a number of eperiments, Planck found the energy density of the radiation emitted by a black body in wavelength interval (, d + was well described
More informationChemistry 24b Lecture 23 Spring Quarter 2004 Instructor: Richard Roberts. (1) It induces a dipole moment in the atom or molecule.
Chemistry 24b Lecture 23 Spring Quarter 2004 Instructor: Richard Roberts Absorption and Dispersion v E * of light waves has two effects on a molecule or atom. (1) It induces a dipole moment in the atom
More informationThe last 2 million years.
Lecture 5: Earth Climate History - Continued Ice core records from both Greenland and Antarctica have produced a remarkable record of climate during the last 450,000 years. Trapped air bubbles provide
More informationMie vs Rayleigh. Sun
Mie vs Rayleigh Sun Chemists Probe Various Energy Levels of Molecules With Appropiate Energy Radiation It is convenient (and accurate enough for our purposes) to treat a molecule or system of molecules
More informationSTSF2223 Quantum Mechanics I
STSF2223 Quantum Mechanics I What is quantum mechanics? Why study quantum mechanics? How does quantum mechanics get started? What is the relation between quantum physics with classical physics? Where is
More informationReflection = EM strikes a boundary between two media differing in η and bounces back
Reflection = EM strikes a boundary between two media differing in η and bounces back Incident ray θ 1 θ 2 Reflected ray Medium 1 (air) η = 1.00 Medium 2 (glass) η = 1.50 Specular reflection = situation
More informationLight carries energy. Lecture 5 Understand Light. Is light. Light as a Particle. ANSWER: Both.
Light carries energy Lecture 5 Understand Light Reading: Chapter 6 You feel energy carried by light when light hits your skin. Energy Conservation: Radiation energy will be given to molecules making your
More informationTananyag fejlesztés idegen nyelven
Tananyag fejlesztés idegen nyelven Prevention of the atmosphere KÖRNYEZETGAZDÁLKODÁSI AGRÁRMÉRNÖKI MSC (MSc IN AGRO-ENVIRONMENTAL STUDIES) Fundamentals in air radition properties Lecture 8 Lessons 22-24
More informationThe Quantum Theory of Atoms and Molecules
The Quantum Theory of Atoms and Molecules Breakdown of classical physics: Wave-particle duality Dr Grant Ritchie Electromagnetic waves Remember: The speed of a wave, v, is related to its wavelength, λ,
More informationATMO 551a Fall Resonant Electromagnetic (EM) Interactions in Planetary atmospheres. Electron transition between different electron orbits
Resonant Electromagnetic (EM) Interactions in Planetary atmospheres There are three classes of energy states that interact with EM radiation that we are interested in to understand how light (EM radiation)
More informationFluoride Laser Crystals: YLiF 4 (YLF)
Chapter 5 Fluoride Laser Crystals: YLiF 4 (YLF) Fluoride crystals are among the most important hosts for laser materials because of their special optical properties. Of these, LiYF 4 (YLF) is one of the
More informationINFRAMET. 2.1 Basic laws
tel: 048 60844873, fax 48 6668780. Basic laws.. Planck law All objects above the temperature of absolute zero emit thermal radiation due to thermal motion of the atoms and the molecules. The hotter they
More informationIntroduction to Spectroscopic methods
Introduction to Spectroscopic methods Spectroscopy: Study of interaction between light* and matter. Spectrometry: Implies a quantitative measurement of intensity. * More generally speaking electromagnetic
More informationStellar Astrophysics: The Continuous Spectrum of Light
Stellar Astrophysics: The Continuous Spectrum of Light Distance Measurement of Stars Distance Sun - Earth 1.496 x 10 11 m 1 AU 1.581 x 10-5 ly Light year 9.461 x 10 15 m 6.324 x 10 4 AU 1 ly Parsec (1
More informationThe Black Body Radiation
The Black Body Radiation = Chapter 4 of Kittel and Kroemer The Planck distribution Derivation Black Body Radiation Cosmic Microwave Background The genius of Max Planck Other derivations Stefan Boltzmann
More informationde = j ν dvdωdtdν. (1)
Transfer Equation and Blackbodies Initial questions: There are sources in the centers of some galaxies that are extraordinarily bright in microwaves. What s going on? The brightest galaxies in the universe
More informationpoint, corresponding to the area it cuts out: θ = (arc length s) / (radius of the circle r) in radians Babylonians:
Astronomische Waarneemtechnieken (Astronomical Observing Techniques) 1 st Lecture: 1 September 11 This lecture: Radiometry Radiative transfer Black body radiation Astronomical magnitudes Preface: The Solid
More informationASTR240: Radio Astronomy
AST24: adio Astronomy HW#1 Due Feb 6, 213 Problem 1 (6 points) (Adapted from Kraus Ch 8) A radio source has flux densities of S 1 12.1 Jy and S 2 8.3 Jy at frequencies of ν 1 6 MHz and ν 2 1415 MHz, respectively.
More informationApplication of IR Raman Spectroscopy
Application of IR Raman Spectroscopy 3 IR regions Structure and Functional Group Absorption IR Reflection IR Photoacoustic IR IR Emission Micro 10-1 Mid-IR Mid-IR absorption Samples Placed in cell (salt)
More informationEquilibrium Properties of Matter and Radiation
Equilibrium Properties of Matter and Radiation Temperature What is it? A measure of internal energy in a system. Measure from (1) velocities of atoms/molecules () population of excited/ionized states (3)
More informationDr. Linlin Ge The University of New South Wales
GMAT 9600 Principles of Remote Sensing Week2 Electromagnetic Radiation: Definition & Physics Dr. Linlin Ge www.gmat.unsw.edu.au/linlinge Basic radiation quantities Outline Wave and quantum properties Polarization
More informationThe Curve of Growth of the Equivalent Width
9 The Curve of Growth of the Equivalent Width Spectral lines are broadened from the transition frequency for a number of reasons. Thermal motions and turbulence introduce Doppler shifts between atoms and
More informationLecture 06. Fundamentals of Lidar Remote Sensing (4) Physical Processes in Lidar
Lecture 06. Fundamentals of Lidar Remote Sensing (4) Physical Processes in Lidar Light interactions with objects (continued) Resonance fluorescence Laser induced fluorescence Doppler effect (Doppler shift
More informationWhat happens when light falls on a material? Transmission Reflection Absorption Luminescence. Elastic Scattering Inelastic Scattering
Raman Spectroscopy What happens when light falls on a material? Transmission Reflection Absorption Luminescence Elastic Scattering Inelastic Scattering Raman, Fluorescence and IR Scattering Absorption
More informationGeneral Considerations 1
General Considerations 1 Absorption or emission of electromagnetic radiation results in a permanent energy transfer from the emitting object or to the absorbing medium. This permanent energy transfer can
More information1 Radiative transfer etc
Radiative transfer etc Last time we derived the transfer equation dτ ν = S ν I v where I ν is the intensity, S ν = j ν /α ν is the source function and τ ν = R α ν dl is the optical depth. The formal solution
More informationASTR-1010: Astronomy I Course Notes Section IV
ASTR-1010: Astronomy I Course Notes Section IV Dr. Donald G. Luttermoser Department of Physics and Astronomy East Tennessee State University Edition 2.0 Abstract These class notes are designed for use
More informationLecture 4: Radiation Transfer
Lecture 4: Radiation Transfer Spectrum of radiation Stefan-Boltzmann law Selective absorption and emission Reflection and scattering Remote sensing Importance of Radiation Transfer Virtually all the exchange
More informationCharacterisation of vibrational modes of adsorbed species
17.7.5 Characterisation of vibrational modes of adsorbed species Infrared spectroscopy (IR) See Ch.10. Infrared vibrational spectra originate in transitions between discrete vibrational energy levels of
More informationLecture 07. Fundamentals of Lidar Remote Sensing (5) Physical Processes in Lidar
Lecture 07. Fundamentals of Lidar Remote Sensing (5) Physical Processes in Lidar Light interaction with objects (continued) Polarization of light Polarization in scattering Comparison of lidar equations
More informationNotes on Black body spectrum
Notes on Black body spectrum Stefano Atzeni October 9, 216 1 The black body Radiation incident on a body can be absorbed, reflected, transmitted. We call black body an ideal body that absorbs all incident
More informationAnalytical Chemistry II
Analytical Chemistry II L4: Signal processing (selected slides) Computers in analytical chemistry Data acquisition Printing final results Data processing Data storage Graphical display https://www.creativecontrast.com/formal-revolution-of-computer.html
More informationFundamental Concepts of Radiation -Basic Principles and Definitions- Chapter 12 Sections 12.1 through 12.3
Fundamental Concepts of Radiation -Basic Principles and Definitions- Chapter 1 Sections 1.1 through 1.3 1.1 Fundamental Concepts Attention is focused on thermal radiation, whose origins are associated
More information