Description of radiation field
|
|
- Baldwin McBride
- 5 years ago
- Views:
Transcription
1 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 empty space. Flux of energy varies in empty space and therefore cannot be the fundamental quantity. L energy time Ex.: Fs = L 4r ˆr r 2 Energy per solid angle works. Assume solar surface emits uniformly Each unit of area on Sun emits Fixed solid angle receives emission from area of r 2. For reference: A = 1 r 2 energy flux solid angle, time ( r r 2 A r )+ independent of r 1 ( r cos A cos )+ 1 r cos A
2 Intensity or radiance lim I ( x,t, ˆn )= 's 0 where t = time = wavelength A = area ˆn E t A = solid angle With I defined this way, radiative transfer in empty space reduces to di = 0, s = distance in ˆn direction (along beam) ds Energy flux In direction ˆn, monochromatic flux is F ˆn = I ( nˆ )ˆ n ˆn d 4 Total flux Fˆn = 0 F ˆn d Comments: *Notice that if I ( nˆ )= I ( nˆ ) then = 0 Fˆn * I ( nˆ )ˆ n is a vector and is a sum of vector components Fˆn F = ê Fê1 1 + ê Fê2 2 + ê Fê3 3 is vector energy flux.
3 *Isotropic radiation I ( x,t, ˆn ) I ( x,t ) No net flux by symmetry. Flux in one direction across surface is of interest. F + = I ( ˆn )ˆn + ˆn d( ˆn ) = I cos 0 0 d ( cos)d = I Notice I < 2 I (whole hemisphere). This result is of special interest because thermalemission from a surface or isotropic scattering from a surface give this geometry. + direction Interaction with matter - Absorption A medium can absorb, emit or scatter radiation. Under absorption alone one expects Energy loss along = Beam *absorption strength *n *s beam distance s intensity per particle # particles vol 1 Since ns = particles, need absorption strength in area I = I ˆ a n s Salby notation
4 Thus di = ˆ I a n I a I Units = length 1 The factor is the absorption coefficient. This attenuation equation is called Lambort's Law. Its integral is di = ds I ln I = s ds + const. I = I ( s 0)e s a ds 0 The "optical path" or "optical depth" u s ()= s a ds 0 has no units. s I () ( ) = s eu I 0 () Transmissivity Comment: Absorption strength is ecpressed in a variety of units. Fundamental combinaion is u. di I = ds = du = ˆ a n ds u is always (strength measure) (gas amount along path) area Strength might be particle, area optical path,. Be careful mass km.amagats
5 Planck intensity spectrum A radiation field inside a container with walls at uniform temperature comes into thermodynamic equilibrium. (It is assumed that the walls have a continuous spectrum of energy transitions that can happen.) This spectrum is the Planck Function. 2h c 2 energy = 5 exp + hc (area)(time)(wave length)(steradian) 1 k T This is energy per unit wavelength. To evaluate,energy per unit frequency use E = = = d d, = c 2h 3 = c 2 exp h 1 k T In practice the first and second radiation constants are used to numerically evaluate. For example: c = 1 5 exp c 2 T 1 Max of is at T = 0.29 cm K. Max of is at T = 0.51 cm K. c 1 = W m 2 c 2 = m K
6
7
8
9 Brightness temperature Thermal emission spectra are often resented in units of brightness temperature. Observe I ( ) radiance units Set I equal to the Planck Function at unknown T b ( T b,)= I Invert, solve for T b ( ). T b ( ) gives the temperature, at each wavelength, that a black surface would need to have in order to emit the observed intensity. ( )
10 Stefan-Boltzmann Law Many surfaces emit approximately the same way that a port in a black cavity would emit. I = ( T,) independent of direction F = F = d = T 4 0 = Wm 2 K 4 Example: Estimate the temperature of a planet. Power received from = a 2 1 A 2 4r = a 2 F s ( ra), F s 1368 W m 2 L Power emitted by planet = 4a 2 T 4 T 4 = 1 A 4 F s T = 254 K = 236 W m2 ( ) A 0.31 a
11 Equation of transfer Thermal emission In the presence of absorption and emission, di ds = I + S Where S is a source term due to emission by the medium. In a region many optical depths across, the exterior boundaries will become unimportant. Then if the region is isothermal, the radiation field will be in thermodynamic equilibrium, with I = B. Then di ds = 0, and I + S = 0 S = B di ds = ( I B ) Emission coefficient = absorption coefficient is Kirchoff s Law.
12 Emission and scattering Denote e exxtinction coefficient. In general e i n i i = monochromatic cross section (lenght) 2 n i = number density of constituent i. Let o be fraction of extinction that scatters into a new direction and is not absorbed. o single scattering albedo. Governing equation di ds = I e ( + J ), ( scat) J ( ˆn )= o P( ˆn, nˆ ) I ( nˆ ) d 4. 4 By o definition, P( ˆn, n ˆ) d 4 = 1 4 ( emission) What is J? Expect C B,if LTE. di ds = I e + 0 P( ˆn, nˆ ) I ( nˆ ) d 4 + C B Deep inside homogeneous region I B (isotropic) and di = 0. Thus ds -B + 0 B P( ˆn, nˆ ) I nˆ ( ) d 4 + C B = 0 Ex. Forward scattering nˆ ˆn
13 C = 1 0 Summary: Kirchoff again 1 di e ds = I + 1 ( 0 )B + 0 P( ˆn, nˆ ) I nˆ 4 ( ) d Intensity change Extinction Emission Scattering Formal integral in absence of scattering Let e ds = dx optical thickness s = 0 s x x =0 I di = I dx B ( T ) (no scattering) e x d e x I dx ( )= B x ( ) dx e x I x = e x 0 B 0 X e x I I x X ( = 0)= e x ( B 0 X ) dx I ( X = 0)= I ( X )e x + x e x B X Intensity emerging Attenuated incident intensity 0 ( ) dx Accumulated emission along path
14
15 Absorption spectrum Transitions In planetary atmospheres transitions between discrete energy levels are of most importance. In stars free-free or bound-free transitions give continuum absorption. absorption lines dominate. h = E Exception: UV and EUV absorption in upper atmosphere. Transitions are Electronic visible Vibrational IR & combinations Rotational far IR Examples of spectra are shown in Salby and in viewgraphs. Units Spectrscopists usually work in frequency units expressed in wave numbers = c ( ) = c s1 = c = 1 (lenght1,usually cm 1 ) wave number Handy identity: ( microns)= 10,00 cm 1 ( )
16 Lorentz line profile In the lower atmosphere, collisional broadening is the most important factor producing frequent dispersion of absorption. Phase coherence of emitted photon is destroyed by collisions. t = time between collisions t Spectrum is broadened by 1 t. 1 1 wave number units c t To estimate, l mfp A n = 1 1 t = l mfp = An A ~ ( 4a 0 ) 2 o, a 0 = Bohr radius ~ 0.5 A m 2 n ~ m 3 Loschmidt's # ~ 300 m s (sound speed) 1 1 An ~ ~ ~3 m 1 t c c =.03 cm 1 Typical IR frequency = 10 microns = 1000 in 1.03 cm -1 Narrow. Since n, Width pressure cm -1
17 The shape is the Lorentz profile f L = L ( ) 2 + L 2 0 0, f L d = 1 0 The cross section is = S f L ( ), S line strength. The strength is a function of temperature S(T ), and L is usually taken to be L = L0 p T 0 p 0 T n, where p 0,T 0 are STP, and n 1 2 and L0 are tabulated in line atlases. Doppler line broadening ~ 350m s1 ~ c ~106 1 m s ~10 6 ~ ~.001 cm 1 Important in upper atmosphere where p small and Lorentz width is small. Doppler shape: D = 2K 0 3 T c m 1 f D = D exp 2 0 0
18 Voigt line profile Convolve Doppler & Lorentz broadening f ( 0 )= f L ( 0 ) f D ( )d There are efficient algorithms to evaluate it See Grody and Yung. Line atlases See the description of the HITRAN, GEISA atlases. Line strength S(T) involves lower state energy. This is because of state population dependence on T. From L TOU, n T S i ( T ) S i ( T r ) T exp hce i 1 r K B T 1 T r n = 2 linear molecule n = 5 2 nonlinear molecule E i = lower state energy for line i T r = 296 K = reference T.
19
20
21
22
23
24
25
26 Plane parallel atmosphere, emission and absorption Transfer eq. in terms of optical depth. d = dz No scattering. di ds = I ( B ) Geometry of ray ds= dz dz cos μ Plane parallel is idealized case = ( z), B = B ( z). Then I = I ( z), 1 di ds = μ di dz = μ di d z \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ ds μ di d = I B Solution for upward intensity I ( z,μ)= I ( s,μ)e + B ( )e ( z) s ( ) μ z μ s μ ( z) d μ μ \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\ z Z = 0
27 Usually I ( s,μ) B ( T s ). In some cases, I ( s,μ) B ( T s ). Where the emissivity varies spectrally but with wide Bands rather than narrow lines. Mars surface mineralogy Is an example. For now, assume B (T s ). Average over a band In practice a finite is of interest. For heating rates can average over spectrum. For remote sensing the instrument has spectral resolution limitations. Average over small enough so that the Plank function ~ constant. I ( z,μ)= 1 B ( T s )e s μ d + 1 s B ( ) e μ d μ where B smooth B ( T s ) 1 e s s μ d B s = B ( z,0,μ)+ B ( z) d z, z,μ dz ( z, z,μ)= 1 e N.B. Sign changes from d dz μ d ( ) d e d μ μ ( ) 1 dz and from reversal of integration range.
Blackbody 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 informationMonday, Oct. 2: Clear-sky radiation; solar attenuation, Thermal. nomenclature
Monday, Oct. 2: Clear-sky radiation; solar attenuation, Thermal nomenclature Sun Earth Y-axis: Spectral radiance, aka monochromatic intensity units: watts/(m^2*ster*wavelength) Blackbody curves provide
More informationAy Fall 2004 Lecture 6 (given by Tony Travouillon)
Ay 122 - Fall 2004 Lecture 6 (given by Tony Travouillon) Stellar atmospheres, classification of stellar spectra (Many slides c/o Phil Armitage) Formation of spectral lines: 1.excitation Two key questions:
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 information2. Illustration of Atmospheric Greenhouse Effect with Simple Models
2. Illustration of Atmospheric Greenhouse Effect with Simple Models In the first lecture, I introduced the concept of global energy balance and talked about the greenhouse effect. Today we will address
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 informationUnderstanding the Greenhouse Effect
EESC V2100 The Climate System spring 200 Understanding the Greenhouse Effect Yochanan Kushnir Lamont Doherty Earth Observatory of Columbia University Palisades, NY 1096, USA kushnir@ldeo.columbia.edu Equilibrium
More informationExample: model a star using a two layer model: Radiation starts from the inner layer as blackbody radiation at temperature T in. T out.
Next, consider an optically thick source: Already shown that in the interior, radiation will be described by the Planck function. Radiation escaping from the source will be modified because the temperature
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 informationOppgavesett kap. 4 (1 av 2) GEF2200
Oppgavesett kap. 4 (1 av 2) GEF2200 hans.brenna@geo.uio.no Exercise 1: Wavelengths and wavenumbers (We will NOT go through this in the group session) What's the relation between wavelength and wavenumber?
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 informationTHREE MAIN LIGHT MATTER INTERRACTION
Chapters: 3and 4 THREE MAIN LIGHT MATTER INTERRACTION Absorption: converts radiative energy into internal energy Emission: converts internal energy into radiative energy Scattering; Radiative energy is
More informationAtmospheric Sciences 321. Science of Climate. Lecture 6: Radiation Transfer
Atmospheric Sciences 321 Science of Climate Lecture 6: Radiation Transfer Community Business Check the assignments Moving on to Chapter 3 of book HW #2 due next Wednesday Brief quiz at the end of class
More informationRadiation 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 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 informationFundamentals of Atmospheric Radiation and its Parameterization
Source Materials Fundamentals of Atmospheric Radiation and its Parameterization The following notes draw extensively from Fundamentals of Atmospheric Physics by Murry Salby and Chapter 8 of Parameterization
More informationATMO 551a Intro to Optical Depth Fall τ υ,z. dz = di υ. B[ v,t(z) ]e
Atmospheric Radiative Transfer We need to understand how energy is transferred via radiation within the atmosphere. We introduce the concept of optical depth. We will further show that the light moves
More informationSources of radiation
Sources of radiation Most important type of radiation is blackbody radiation. This is radiation that is in thermal equilibrium with matter at some temperature T. Lab source of blackbody radiation: hot
More informationRadiative Equilibrium Models. Solar radiation reflected by the earth back to space. Solar radiation absorbed by the earth
I. The arth as a Whole (Atmosphere and Surface Treated as One Layer) Longwave infrared (LWIR) radiation earth to space by the earth back to space Incoming solar radiation Top of the Solar radiation absorbed
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 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 informationBeer-Lambert (cont.)
The Beer-Lambert Law: Optical Depth Consider the following process: F(x) Absorbed flux df abs F(x + dx) Scattered flux df scat x x + dx The absorption or scattering of radiation by an optically active
More informationSIMPLE RADIATIVE TRANSFER
ASTR 511/O Connell Lec 4 1 SIMPLE RADIATIVE TRANSFER The theory of radiative transfer provides the means for determining the emergent EM spectrum of a cosmic source and also for describing the effects
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 informationEarth: the Goldilocks Planet
Earth: the Goldilocks Planet Not too hot (460 C) Fig. 3-1 Not too cold (-55 C) Wave properties: Wavelength, velocity, and? Fig. 3-2 Reviewing units: Wavelength = distance (meters or nanometers, etc.) Velocity
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 informationOutline. Today we will learn what is thermal radiation
Thermal Radiation & Outline Today we will learn what is thermal radiation Laws Laws of of themodynamics themodynamics Radiative Radiative Diffusion Diffusion Equation Equation Thermal Thermal Equilibrium
More informationSISD Training Lectures in Spectroscopy
SISD Training Lectures in Spectroscopy Anatomy of a Spectrum Visual Spectrum of the Sun Blue Spectrum of the Sun Morphological Features in Spectra λ 2 Line Flux = Fλ dλ λ1 (Units: erg s -1 cm -2 ) Continuum
More informationThe mathematics of scattering and absorption and emission
The mathematics of scattering and absorption and emission The transmittance of an layer depends on its optical depth, which in turn depends on how much of the substance the radiation has to pass through,
More informationObservations 3: Data Assimilation of Water Vapour Observations at NWP Centres
Observations 3: Data Assimilation of Water Vapour Observations at NWP Centres OUTLINE: Data Assimilation A simple analogy: data fitting 4D-Var The observation operator : RT modelling Review of Radiative
More informationRadiation from planets
Chapter 4 Radiation from planets We consider first basic, mostly photometric radiation parameters for solar system planets which can be easily compared with existing or future observations of extra-solar
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 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 information2 The Radiative Transfer Equation
9 The Radiative Transfer Equation. Radiative transfer without absorption and scattering Free space or homogeneous space I (r,,) I (r,,) r -r d da da Figure.: Following a pencil of radiation in free space
More informationLet s make a simple climate model for Earth.
Let s make a simple climate model for Earth. What is the energy balance of the Earth? How is it controlled? ó How is it affected by humans? Energy balance (radiant energy) Greenhouse Effect (absorption
More informationToday. Kirchoff s Laws. Emission and Absorption. Stellar Spectra & Composition. Doppler Effect & Motion. Extrasolar Planets
Today Kirchoff s Laws Emission and Absorption Stellar Spectra & Composition Doppler Effect & Motion Extrasolar Planets Three basic types of spectra Continuous Spectrum Intensity Emission Line Spectrum
More informationStars AS4023: Stellar Atmospheres (13) Stellar Structure & Interiors (11)
Stars AS4023: Stellar Atmospheres (13) Stellar Structure & Interiors (11) Kenneth Wood, Room 316 kw25@st-andrews.ac.uk http://www-star.st-and.ac.uk/~kw25 What is a Stellar Atmosphere? Transition from dense
More informationSummary of radiation in participating media
Emission, absorption, scattering Summary of radiation in participating media Governing equations (Chapter 9) Over a distance ds, the spectral intensity I η (watts per m 2 of cross-sectional area per steradian
More informationAT622 Section 3 Basic Laws
AT6 Section 3 Basic Laws There are three stages in the life of a photon that interest us: first it is created, then it propagates through space, and finally it can be destroyed. The creation and destruction
More informationATMO/OPTI 656b Spring 2009
Nomenclature and Definition of Radiation Quantities The various Radiation Quantities are defined in Table 2-1. Keeping them straight is difficult and the meanings may vary from textbook to textbook. I
More informationWeighting Functions and Atmospheric Soundings: Part I
Weighting Functions and Atmospheric Soundings: Part I Ralf Bennartz Cooperative Institute for Meteorological Satellite Studies University of Wisconsin Madison Outline What we want to know and why we need
More informationChapter 4. Spectroscopy. Dr. Tariq Al-Abdullah
Chapter 4 Spectroscopy Dr. Tariq Al-Abdullah Learning Goals: 4.1 Spectral Lines 4.2 Atoms and Radiation 4.3 Formation of the Spectral Lines 4.4 Molecules 4.5 Spectral Line Analysis 2 DR. T. AL-ABDULLAH
More informationBlackbody Radiation. A substance that absorbs all incident wavelengths completely is called a blackbody.
Blackbody Radiation A substance that absorbs all incident wavelengths completely is called a blackbody. What's the absorption spectrum of a blackbody? Absorption (%) 100 50 0 UV Visible IR Wavelength Blackbody
More informationToday. Spectra. Thermal Radiation. Wien s Law. Stefan-Boltzmann Law. Kirchoff s Laws. Emission and Absorption. Spectra & Composition
Today Spectra Thermal Radiation Wien s Law Stefan-Boltzmann Law Kirchoff s Laws Emission and Absorption Spectra & Composition Spectrum Originally, the range of colors obtained by passing sunlight through
More information2. NOTES ON RADIATIVE TRANSFER The specific intensity I ν
1 2. NOTES ON RADIATIVE TRANSFER 2.1. The specific intensity I ν Let f(x, p) be the photon distribution function in phase space, summed over the two polarization states. Then fdxdp is the number of photons
More informationAtomic Physics 3 ASTR 2110 Sarazin
Atomic Physics 3 ASTR 2110 Sarazin Homework #5 Due Wednesday, October 4 due to fall break Test #1 Monday, October 9, 11-11:50 am Ruffner G006 (classroom) You may not consult the text, your notes, or any
More information6. Interstellar Medium. Emission nebulae are diffuse patches of emission surrounding hot O and
6-1 6. Interstellar Medium 6.1 Nebulae Emission nebulae are diffuse patches of emission surrounding hot O and early B-type stars. Gas is ionized and heated by radiation from the parent stars. In size,
More informationSubstellar Atmospheres II. Dust, Clouds, Meteorology. PHY 688, Lecture 19 Mar 11, 2009
Substellar Atmospheres II. Dust, Clouds, Meteorology PHY 688, Lecture 19 Mar 11, 2009 Outline Review of previous lecture substellar atmospheres: opacity, LTE, chemical species, metallicity Dust, Clouds,
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 informationChapter 5 Light and Matter: Reading Messages from the Cosmos. How do we experience light? Colors of Light. How do light and matter interact?
Chapter 5 Light and Matter: Reading Messages from the Cosmos How do we experience light? The warmth of sunlight tells us that light is a form of energy We can measure the amount of energy emitted by a
More informationINTRODUCTION TO MICROWAVE REMOTE SENSING - II. Dr. A. Bhattacharya
1 INTRODUCTION TO MICROWAVE REMOTE SENSING - II Dr. A. Bhattacharya The Radiation Framework The information about features on the Earth s surface using RS depends on measuring energy emanating from the
More informationAtmospheric "greenhouse effect" - How the presence of an atmosphere makes Earth's surface warmer
Atmospheric "greenhouse effect" - How the presence of an atmosphere makes Earth's surface warmer Some relevant parameters and facts (see previous slide sets) (So/) 32 W m -2 is the average incoming solar
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 informationRadiation Transport in a Gas
Radiation Transport in a Gas By analogy to a particle gas, define a photon distribution function by, f ν ν, Ω; r, t)dvdωd r = Number of photons of a frequency in ν, ν + dν), in a volume at rd r), with
More information1. Radiative Transfer. 2. Spectrum of Radiation. 3. Definitions
1. Radiative Transfer Virtually all the exchanges of energy between the earth-atmosphere system and the rest of the universe take place by radiative transfer. The earth and its atmosphere are constantly
More informationAtmospheric Radiation
Atmospheric Radiation NASA photo gallery Introduction The major source of earth is the sun. The sun transfer energy through the earth by radiated electromagnetic wave. In vacuum, electromagnetic waves
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 informationP607 Climate and Energy (Dr. H. Coe)
P607 Climate and Energy (Dr. H. Coe) Syllabus: The composition of the atmosphere and the atmospheric energy balance; Radiative balance in the atmosphere; Energy flow in the biosphere, atmosphere and ocean;
More informationStefan-Boltzmann law for the Earth as a black body (or perfect radiator) gives:
2. Derivation of IPCC expression ΔF = 5.35 ln (C/C 0 ) 2.1 Derivation One The assumptions we will make allow us to represent the real atmosphere. This remarkably reasonable representation of the real atmosphere
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 information1. Weather and climate.
Lecture 31. Introduction to climate and climate change. Part 1. Objectives: 1. Weather and climate. 2. Earth s radiation budget. 3. Clouds and radiation field. Readings: Turco: p. 320-349; Brimblecombe:
More informationMARYLAND. Fundamentals of heat transfer Radiative equilibrium Surface properties Non-ideal effects. Conduction Thermal system components
Fundamentals of heat transfer Radiative equilibrium Surface properties Non-ideal effects Internal power generation Environmental temperatures Conduction Thermal system components 2003 David L. Akin - All
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 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 informationElectromagnetic Spectra. AST443, Lecture 13 Stanimir Metchev
Electromagnetic Spectra AST443, Lecture 13 Stanimir Metchev Administrative Homework 2: problem 5.4 extension: until Mon, Nov 2 Reading: Bradt, chapter 11 Howell, chapter 6 Tenagra data: see bottom of Assignments
More informationaka Light Properties of Light are simultaneously
Today Interaction of Light with Matter Thermal Radiation Kirchhoff s Laws aka Light Properties of Light are simultaneously wave-like AND particle-like Sometimes it behaves like ripples on a pond (waves).
More informationASTRONOMY 103: THE EVOLVING UNIVERSE. Lecture 4 COSMIC CHEMISTRY Substitute Lecturer: Paul Sell
ASTRONOMY 103: THE EVOLVING UNIVERSE Lecture 4 COSMIC CHEMISTRY Substitute Lecturer: Paul Sell Two Blackbody Trends 1. Wein s (Veen s) Law λp 1 / T or λp = 2900 / T (λp is the peak wavelength in micrometers
More informationWhich picture shows the larger flux of blue circles?
Which picture shows the larger flux of blue circles? 33% 33% 33% 1. Left 2. Right 3. Neither Left Right Neither This Week: Global Climate Model Pt. 1 Reading: Chapter 3 Another Problem Set Coming Towards
More informationHand in Question sheets with answer booklets Calculators allowed Mobile telephones or other devices not allowed
York University Department of Earth and Space Science and Engineering ESSE 3030 Department of Physics and Astronomy PHYS 3080 Atmospheric Radiation and Thermodynamics Final Examination 2:00 PM 11 December
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 informationRadiative Transfer Multiple scattering: two stream approach 2
Radiative Transfer Multiple scattering: two stream approach 2 N. Kämpfer non Institute of Applied Physics University of Bern 28. Oct. 24 Outline non non Interpretation of some specific cases Semi-infinite
More informationSome fundamentals. Statistical mechanics. The non-equilibrium ISM. = g u
Some fundamentals Statistical mechanics We have seen that the collision timescale for gas in this room is very small relative to radiative timesscales such as spontaneous emission. The frequent collisions
More informationRadiation processes and mechanisms in astrophysics I. R Subrahmanyan Notes on ATA lectures at UWA, Perth 18 May 2009
Radiation processes and mechanisms in astrophysics I R Subrahmanyan Notes on ATA lectures at UWA, Perth 18 May 009 Light of the night sky We learn of the universe around us from EM radiation, neutrinos,
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 informationTHE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES DAVID F. GRAY University of Western Ontario, London, Ontario, Canada CAMBRIDGE UNIVERSITY PRESS Contents Preface to the first edition Preface to the
More informationIntroduction to Electromagnetic Radiation and Radiative Transfer
Introduction to Electromagnetic Radiation and Radiative Transfer Temperature Dice Results Visible light, infrared (IR), ultraviolet (UV), X-rays, γ-rays, microwaves, and radio are all forms of electromagnetic
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 informationAstronomy 421. Lecture 14: Stellar Atmospheres III
Astronomy 421 Lecture 14: Stellar Atmospheres III 1 Lecture 14 - Key concepts: Spectral line widths and shapes Curve of growth 2 There exists a stronger jump, the Lyman limit, occurring at the wavelength
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 informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 11:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
More informationThursday, November 1st.
Thursday, November 1st. Announcements. Homework 7 - due Tuesday, Nov. 6 Homework 8 - paper 2 topics, questions and sources due Tuesday, Nov. 13 Midterm Paper 2 - due Tuesday, Nov. 20 I will hand out a
More informationThe formation of stars and planets. Day 1, Topic 2: Radiation physics. Lecture by: C.P. Dullemond
The formation of stars and planets Day 1, Topic 2: Radiation physics Lecture by: C.P. Dullemond Astronomical Constants CGS units used throughout lecture (cm,erg,s...) AU = Astronomical Unit = distance
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 informationTake away concepts. What is Energy? Solar Radiation Emission and Absorption. Energy: The ability to do work
Solar Radiation Emission and Absorption Take away concepts 1. 2. 3. 4. 5. 6. Conservation of energy. Black body radiation principle Emission wavelength and temperature (Wien s Law). Radiation vs. distance
More informationLecture 2 Solutions to the Transport Equation
Lecture 2 Solutions to the Transport Equation Equation along a ray I In general we can solve the static transfer equation along a ray in some particular direction. Since photons move in straight lines
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 informationAssignments. For Wed. 1 st Midterm is Friday, Oct. 12. Do Online Exercise 08 ( Doppler shift tutorial)
Assignments For Wed. Do Online Exercise 08 ( Doppler shift tutorial) 1 st Midterm is Friday, Oct. 12 Chapter 5 Light: The Cosmic Messenger Which forms of light are lower in energy and frequency than the
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 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 informationSpontaneous Emission, Stimulated Emission, and Absorption
Chapter Six Spontaneous Emission, Stimulated Emission, and Absorption In this chapter, we review the general principles governing absorption and emission of radiation by absorbers with quantized energy
More informationWhat are the three basic types of spectra?
Learning from Light Our goals for learning What are the three basic types of spectra? How does light tell us what things are made of? How does light tell us the temperatures of planets and stars? How do
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 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 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 informationRadiative Transfer and Molecular Lines Sagan Workshop 2009
Radiative Transfer and Molecular Lines Sagan Workshop 2009 Sara Seager Trent Schindler Trent Schindler MIT Lecture Contents Overview of Equations for Planetary Atmospheres Radiative Transfer Thermal Inversions
More informationBasic Properties of Radiation, Atmospheres, and Oceans
Basic Properties of Radiation, Atmospheres, and Oceans Jean-Sébastian Tempel Department of Physics and Technology University of Bergen 16. Mai 2007 phys264 - Environmental Optics and Transport of Light
More informationRadiation in climate models.
Lecture. Radiation in climate models. Objectives:. A hierarchy of the climate models.. Radiative and radiative-convective equilibrium.. Examples of simple energy balance models.. Radiation in the atmospheric
More informationThe Main Point. How do light and matter interact? Lecture #7: Radiation and Spectra II. How is light absorbed and emitted?
Lecture #7: Radiation and Spectra II How is light absorbed and emitted? Models of Atomic Structure. Formation of Spectral Lines. Doppler Shift. Applications in Solar System Studies Detecting gaseous phases
More informationThe current climate epoch: The Holocene
Lecture 1: Climate and the 1st Law of Thermodynamics Quick Review of Monday s main features: Lapse rate, Hydrostatic Balance surface = 288K (15 C). In lowest 10 km, the lapse rate, Γ, averages: T Γ
More informationLecture Notes Prepared by Mike Foster Spring 2007
Lecture Notes Prepared by Mike Foster Spring 2007 Solar Radiation Sources: K. N. Liou (2002) An Introduction to Atmospheric Radiation, Chapter 1, 2 S. Q. Kidder & T. H. Vander Haar (1995) Satellite Meteorology:
More information