1. Radiative Transfer. 2. Spectrum of Radiation. 3. Definitions
|
|
- Barrie Payne
- 7 years ago
- Views:
Transcription
1 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 absorbing solar radiation and emitting their own radiation to space. Over a long period of time, the rates of absorption and emission are very nearly equal, thus the earth-atmosphere system is very nearly in equilibrium with the sun. Radiative transfer also serves as a mechanism for exchanging energy between the atmosphere and the underlying surface, and among different layers of the atmosphere. Radiative transfer plays an important role in a number of chemical reactions in the upper atmosphere and in the formation of photochemical smogs. The transfer properties of visible radiation determine the visibility, the color of the sky and the appearance of clouds. Radiation emitted by the earth and atmosphere and intercepted by satellites is the basis for remote sensing of the atmospheric temperature structure, water vapor amounts, ozone and other trace gases. 2. Spectrum of Radiation Electromagnetic radiation may be viewed as an ensemble of waves propagating at the speed of light (c = m/s through vacum). We characterize radiation in terms of: frequency ν = c /λ wavelength λ = c /ν Radiative transfer in planetary atmosphere involves an ensemble of waves with a continuum of wavelengths and frequencies. We partition them into bands : shortwave (λ < 4µm) carries most of the energy associated with solar radiation or longwave (λ > 4µm) which refers to the band that encompasses most of the terrestrial. The visible region µm is defined by the range of wavelengths that the human eye is capable of sensing, and subranges of the visible are discernible as colors. 3. Definitions Solid Angle ω Consider a cone with its vertex at the origin of a concentric spherical surface. The solid angle is defined as the ratio of the area of the sphere 1
2 Figure 1: Ahrens, Chapter 2 2
3 intercepted by the cone to the square of the radius. ω = A r 2 (1) In spherical coordinates dω = da r 2 (2) da = r 2 sinθdθdφ (3) The unit of the solid angle is the steradian. The area cut out of a sphere by one steradian is equal to the square of the radius. Integration over the entire spherical surface then gives ω = 4πsteradians Monochromatic flux density F λ Amount of radiant energy with a given wavelength passing through a unit area per unit time. Expressed in [W m 2 ]. Total flux density is calculated as the integral over all wavelengths F = λ2 λ 1 F λ dλ = ν 2 ν 1 F ν dν. Monochromatic Intensity (or Monochromatic Radiance) I λ Radiant energy in a specific wavelength per unit time coming from a specific direction and passing through a unit area perpendicular to that direction. Total intensity is calculated as the integral over all wavelengths I = λ 2 λ 1 I λ dλ = ν 2 ν 1 I ν dν. The units are [W m 2 steradian 1 ].The intensity I λ and flux density F λ are related by I λ = df (4) dωcosθ We can integrate over the solid angle subtended by a hemisphere to determine the monochromatic flux density coming from all directions F λ = 2πsteradians 4. Blackbody Radiation 0 I λ cosθdω = 2π 0 dφ π/2 A blackbody is a surface that absorbs all incident radiation. 0 I λ cosθsinφdφ (5) 3
4 The Planck Function Determined experimentally, the intensity of radiation emitted by a blackbody is c 1 λ 5 B λ = (6) π(e c 2/λT 1) where c 1 = W m 2 and c 2 = mk. Theoretical justification of this empirical relationship led to the development of the theory of quantum physics. Wien s Displacement Law Differentiating Equation 6 and setting the derivative equal to zero, gives the wavelength of peak emission for a blackbody at temperature T (HW6). λ m = 2897 (7) T where T in K and λ m in µm. An important consequence of Wien displacement law is the fact that solar radiation is concentrated in the visible and near-infrared parts of the spectrum, while radiation emitted by the planets and their atmospheres is largely confined to the infrared. The nearly complete absence of overlap between the curves justifies dealing with solar and planetary radiation separately in many problems of radiative transfer. Stefan-Boltzmann Law The black body flux density obtained by integrating the Planck function πb λ over all wavelengths. F = σt 4 (8) Where σ is the Stefan-Boltzmann constant equal to W m 2 K 4 4
5 5. Radiative properties of Nonblack materials Unlike blackbodies, which absorb all incident radiation, nonblack bodies such as gaseous media can also reflect and transmit radiation. We will give a brief description of the radiative processes in nonblack bodies. The fate of radiation depends on wavelength. 1. Transmitted Radiation passes undisturbed. We define the monochromatic fractional transmissivity as T λ = I λ(transmitted) I λ (incident) 2. Reflected Radiation. Reflectivity is depicted by albedo. Albedo usually represents all wavelengths and refers to the earth-atmosphere reflection. We define the monochromatic fractional reflectivity as R λ = I λ(transmitted) I λ (incident) 3. Absorbed Increase in internal energy of the object. We define the monochromatic fractional absorptivity as α λ = I λ(absorbed) I λ (incident) (a) Ionization-Dissociation Interactions. In these interactions, an electron is stripped from an atom or molecule, or a molecule is torn apart. These interactions occur primarily at ultraviolet and shorter wavelengths. All solar radiation shorter than about 0.1 µm in wavelength is absorbed in the upper atmosphere by ionizing atmospheric gases, particularly atomic oxygen. Between 0.1 and 0.2 µm molecular oxygen dissociates into atomic oxygen. Radiation between 0.2 and 0.3 µm is absorbed by dissociation of ozone. These bands are important for preventing the radiation from reaching the ground and in satellite meteorology for measuring ozone concentrations. (b) Electronic Transitions Orbital electron jumps between quantized energy levels. These occur mostly in the UV and visible. Ozone, and molecular oxygen. (c) Vibrational transitions A molecule changes vibrational energy states. These transitions occur mostly in the infrared portion of the spectrum and are extremely important for satellite meteorology. The two chief absorbers in the infrared region of the spectrum are carbon dioxide and water vapor. Symmetric stretching has neither a static or dynamic electric dipole moment because the symmetry of the molecule is maintained. If a molecule has no electric dipole moment, the electric field of incident radiation cannot interact with the molecule. (This is why 5
6 N 2 and O 2, the two most abundant gases in the atmosphere, are transparent in the infrared. (d) Rotational transitions a molecule changes rotational states. These occur in the far infrared and microwave portion of the spectrum. They can occur at the same time as vibrational transitions. Figure 4.7. The three are related by α λ + R λ + T λ = 1. For a black body α λ = 1. 5a. Other Definitions Total Mass Extinction Coefficient If a beam of intensity I λ becomes I λ + di λ upon traversing a distance ds in its direction of propagation through a medium of density ρ, then the reduction of intensity due to extinction (which could be absorption, reflection, scattering, diffraction, refraction etc.) is di λ = k λt ρi λ ds (9) where k λt is the total mass extinction coefficient and has units [m 2 kg 1 ]. We define the optical depth τ λ in terms of the total mass extinction coefficient as follows: τ λ = s 0 k λt ρds Mass Absorpion Coefficient If a beam of intensity I λ becomes I λ + di λ upon traversing a distance ds in its direction of propagation through a medium of density ρ, then the reduction of intensity due to absorption is: di λ = k λa ρi λ ds (10) where k λa is the mass absorption coefficient and has units [m 2 kg 1 ]. We define the absorption optical depth τ λa as τ λa = s 0 k λaρds Mass Scattering Coefficient If a beam of intensity I λ becomes I λ + di λ upon traversing a distance ds in its direction of propagation through a medium of density ρ, then the reduction of intensity due to scattering is: di λ = k λs ρi λ ds (11) where k λs is the mass scattering coefficient and has units [m 2 kg 1 ]. We define the scattering optical depth τ λs as τ λs = s 0 k λsρds It follows that k λt = k λa + k λs 6
7 5b. Kirchoff s Law It can be shown that the radiation emitted by a given material is a function of temperature and wavelength only. Consider an opaque, hollow enclosure with zero transmissivity into which is placed a slab of finite thickness. In general, this slab will reflect, absorb and transmit parts of the incident radiation. In addition, it will emit radiation itself. We now allow the enclosure and the slab to reach thermodynamic equilibrium, such that the slab and the enclosure walls are the same temperature. Under this condition, the flow of energy in all directions must be the same. In thermodynamic equilibrium, the amount entering the slab must exactly equal the amount leaving, or there would be a net flow of heat to or from the walls, into or out of the slab. Since the slab and the walls are in thermodynamic equilibrium, this would constitute a violation of the Second Law of Thermodynamics. Therefore, the balance equation is: I λ R λ I λ = T λ I λ + E λ (12) Where E λ is the emitted radiance in the same direction as I λ. But T λ I λ = I λ (1 α λ R λ ) since α λ + R λ + T λ = 1. Therefore, I λ (1 R λ ) = I λ (1 α λ R λ ) + E λ (13) Thus, E λ α λ I λ = 0 or E λ = α λ I λ Thus, inside of an opaque, hollow enclosure in thermodynamic equilibrium, the amount emitted by the slab equals the amount absorbed by the slab. We now imagine our enclosure to be replaced by a different one, constructed from a different material, and again allow it to come into thermodynamic equilibrium with the same slab and at the same temperature as before. Consequently, the slab emission will be the same as before, since it depends only on temperature and wavelength, neither of which has been changed. Similarly, the slab absorption will not change because the slab material is the same. Thus we have: E λ = α λ I λ (14) Where I λ is the incident radiation on the slab in the new enclosure, thus it follows that I λ = I λ.thus, the radiation within an opaque, hollow enclosure is independent of the material from which the walls are made. Re-writing the above E equation we see λ = I α l ambda λb = f(t, λ) only and I λb is the radiance inside an opaque hollow enclosure at temperature T and wavelength λ. 7
8 This result is known as Kirchhoff s Law, which states that The ratio of the emission to the fractional absorptivity of a slab of any material in a state of thermodynamic equilibrium and at wavelength λ is equal to a constant. We may now define the fractional emissivity ɛ λ as the ratio of the radiation emitted at the wavelength λ to that within a hollow enclosure at the same temperature or: ɛ λ = E λ I λb (15) From this definition, we see that E λ = ɛ λ I λb. But from Kirchoff s Law it then follows: ɛ λ = α λ (16) Or the fractional emissivity equals the fractional absorptivity Kirchoff s Law is fundamental to further development of the subject of radiative transfer, and is frequently applied in a variety of applications. Recalling that it is strictly valid only under conditions of thermodynamic equilibrium, it is nevertheless generally assumed to be valid for atmospheric problems even though the atmosphere is not strictly in thermodynamic equilibrium. We may now carry this thought experiment one step further. Let s replace this slab by an ideal black body such that, by definition, it completely absorbs all radiation falling on it. Inside the hollow enclosure then, the radiation leaving the black body slab consists entirely of radiation emitted by the slab. The equilibrium condition becomes I λb = E λ (17) leading to the important conclusion that the radiation flowing in any direction within the hollow enclosure in thermodynamic equilibrium is equal to the energy emitted in the same direction as an ideal black body. Such radiation is called black body radiation, and from our earlier arguments is isotropic or equal in all directions. 8
9 6. Examples 1. Prove that the intensity I of solar radiation is independent of distance from the sun, provided that the distance is large and that radiation emitted from each elemental area on the sun is independent of the zenith angle. 2. The average flux density F e of solar radiation reaching the earth s orbit is 1370W m 2. Nearly all the radiation is emitted from the outermost visible layer of the sun, which has a mean radius of m. Calculate the equivalent blackbody temperature or effective temperature of this layer. The mean distance between the earth and sun is m. 3. Calculate the equivalent blackbody temperature of the earth assuming a planetary albedo α p = 0.3 where α p is the fraction of the total incident solar radiation that is reflected and scattered back to space. Assume that the earth is in radiative equilibrium. 4. A completely gray flat surface on the moon with an absorptivity of 0.9 is exposed to direct overhead solar radiation. What is the radiative equilibrium temperature of the surface? If the actual temperature is 300K, what is the net flux density above the surface? 5. A flat surface is subject to overhead solar radiation as in the previous example. The absorptivity is 0.1 for solar radiation and 0.8 in the infrared part of the spectrum, where most of the emission takes place. Compute the radiative equilibrium temperature. 6. Calculate the radiative equilibrium temperature of the earth s surface and atmosphere assuming that the atmosphere can be regarded as a thin layer with absorptivity of 0.1 for solar radiation and 0.8 for terrestrial radiation. Assume that the earth s surface radiates as a black body. 9
Solar Flux and Flux Density. Lecture 3: Global Energy Cycle. Solar Energy Incident On the Earth. Solar Flux Density Reaching Earth
Lecture 3: Global Energy Cycle Solar Flux and Flux Density Planetary energy balance Greenhouse Effect Vertical energy balance Latitudinal energy balance Seasonal and diurnal cycles Solar Luminosity (L)
More informationRadiation Transfer in Environmental Science
Radiation Transfer in Environmental Science with emphasis on aquatic and vegetation canopy media Autumn 2008 Prof. Emmanuel Boss, Dr. Eyal Rotenberg Introduction Radiation in Environmental sciences Most
More informationChapter 2. The global energy balance. 2.1 Planetary emission temperature
Chapter 2 The global energy balance We consider now the general problem of the radiative equilibrium temperature of the Earth. The Earth is bathed in solar radiation and absorbs much of that incident upon
More informationOverview. What is EMR? Electromagnetic Radiation (EMR) LA502 Special Studies Remote Sensing
LA502 Special Studies Remote Sensing Electromagnetic Radiation (EMR) Dr. Ragab Khalil Department of Landscape Architecture Faculty of Environmental Design King AbdulAziz University Room 103 Overview What
More informationPrinciple of Thermal Imaging
Section 8 All materials, which are above 0 degrees Kelvin (-273 degrees C), emit infrared energy. The infrared energy emitted from the measured object is converted into an electrical signal by the imaging
More information5. The Nature of Light. Does Light Travel Infinitely Fast? EMR Travels At Finite Speed. EMR: Electric & Magnetic Waves
5. The Nature of Light Light travels in vacuum at 3.0. 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien s Law & the Stefan-Boltzmann Law Light has
More informationCorso di Fisica Te T cnica Ambientale Solar Radiation
Solar Radiation Solar radiation i The Sun The Sun is the primary natural energy source for our planet. It has a diameter D = 1.39x10 6 km and a mass M = 1.989x10 30 kg and it is constituted by 1/3 of He
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 information2 Absorbing Solar Energy
2 Absorbing Solar Energy 2.1 Air Mass and the Solar Spectrum Now that we have introduced the solar cell, it is time to introduce the source of the energy the sun. The sun has many properties that could
More informationChapter 2: Solar Radiation and Seasons
Chapter 2: Solar Radiation and Seasons Spectrum of Radiation Intensity and Peak Wavelength of Radiation Solar (shortwave) Radiation Terrestrial (longwave) Radiations How to Change Air Temperature? Add
More informationESCI 107/109 The Atmosphere Lesson 2 Solar and Terrestrial Radiation
ESCI 107/109 The Atmosphere Lesson 2 Solar and Terrestrial Radiation Reading: Meteorology Today, Chapters 2 and 3 EARTH-SUN GEOMETRY The Earth has an elliptical orbit around the sun The average Earth-Sun
More informationElectromagnetic Radiation (EMR) and Remote Sensing
Electromagnetic Radiation (EMR) and Remote Sensing 1 Atmosphere Anything missing in between? Electromagnetic Radiation (EMR) is radiated by atomic particles at the source (the Sun), propagates through
More informationSolar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation
Outline MAE 493R/593V- Renewable Energy Devices Solar Energy Electromagnetic wave Solar spectrum Solar global radiation Solar thermal energy Solar thermal collectors Solar thermal power plants Photovoltaics
More informationTeaching Time: One-to-two 50-minute periods
Lesson Summary Students create a planet using a computer game and change features of the planet to increase or decrease the planet s temperature. Students will explore some of the same principles scientists
More informationBlackbody radiation derivation of Planck s radiation low
Blackbody radiation derivation of Planck s radiation low 1 Classical theories of Lorentz and Debye: Lorentz (oscillator model): Electrons and ions of matter were treated as a simple harmonic oscillators
More informationCHAPTER 3 ABSORPTION, EMISSION, REFLECTION, AND SCATTERING
CHAPTER 3 ABSORPTION, EMISSION, REFLECTION, AND SCATTERING 3.1 Absorption and Emission As noted earlier, blackbody radiation represents the upper limit to the amount of radiation that a real substance
More informationTreasure Hunt. Lecture 2 How does Light Interact with the Environment? EMR Principles and Properties. EMR and Remote Sensing
Lecture 2 How does Light Interact with the Environment? Treasure Hunt Find and scan all 11 QR codes Choose one to watch / read in detail Post the key points as a reaction to http://www.scoop.it/t/env202-502-w2
More informationClouds and the Energy Cycle
August 1999 NF-207 The Earth Science Enterprise Series These articles discuss Earth's many dynamic processes and their interactions Clouds and the Energy Cycle he study of clouds, where they occur, and
More informationCHAPTER 2 Energy and Earth
CHAPTER 2 Energy and Earth This chapter is concerned with the nature of energy and how it interacts with Earth. At this stage we are looking at energy in an abstract form though relate it to how it affect
More informationTOPIC 5 (cont.) RADIATION LAWS - Part 2
TOPIC 5 (cont.) RADIATION LAWS - Part 2 Quick review ELECTROMAGNETIC SPECTRUM Our focus in this class is on: UV VIS lr = micrometers (aka microns) = nanometers (also commonly used) Q1. The first thing
More informationTake away concepts. What is Energy? Solar Energy. EM Radiation. Properties of waves. Solar Radiation Emission and Absorption
Take away concepts Solar Radiation Emission and Absorption 1. 2. 3. 4. 5. 6. Conservation of energy. Black body radiation principle Emission wavelength and temperature (Wein s Law). Radiation vs. distance
More informationa) species of plants that require a relatively cool, moist environment tend to grow on poleward-facing slopes.
J.D. McAlpine ATMS 611 HMWK #8 a) species of plants that require a relatively cool, moist environment tend to grow on poleward-facing slopes. These sides of the slopes will tend to have less average solar
More informationENERGY & ENVIRONMENT
Greenhouse molecules, their spectra and function in the atmosphere by Jack Barrett Reprinted from ENERGY & ENVIRNMENT VLUME 16 No. 6 2005 MULTI-SCIENCE PUBLISING C. LTD. 5 Wates Way, Brentwood, Essex CM15
More informationBlackbody Radiation References INTRODUCTION
Blackbody Radiation References 1) R.A. Serway, R.J. Beichner: Physics for Scientists and Engineers with Modern Physics, 5 th Edition, Vol. 2, Ch.40, Saunders College Publishing (A Division of Harcourt
More informationThe Earth s Atmosphere
THE SUN-EARTH SYSTEM III The Earth s Atmosphere Composition and Distribution of the Atmosphere The composition of the atmosphere and the way its gases interact with electromagnetic radiation determine
More informationPassive Remote Sensing of Clouds from Airborne Platforms
Passive Remote Sensing of Clouds from Airborne Platforms Why airborne measurements? My instrument: the Solar Spectral Flux Radiometer (SSFR) Some spectrometry/radiometry basics How can we infer cloud properties
More informationD.S. Boyd School of Earth Sciences and Geography, Kingston University, U.K.
PHYSICAL BASIS OF REMOTE SENSING D.S. Boyd School of Earth Sciences and Geography, Kingston University, U.K. Keywords: Remote sensing, electromagnetic radiation, wavelengths, target, atmosphere, sensor,
More informationThe Surface Energy Budget
The Surface Energy Budget The radiation (R) budget Shortwave (solar) Radiation Longwave Radiation R SW R SW α α = surface albedo R LW εσt 4 ε = emissivity σ = Stefan-Boltzman constant T = temperature Subsurface
More informationLight as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation
The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered
More informationI ν = λ 2 I λ. λ<0.35 µm F λ =0 0.70 µm <λ<1.00 µm F λ =0.2 Wm 2 µm 1. λ>1.00 µm F λ =0. F λi 4λ i. i 1
Chapter 4 4.12 Remote sensing in the microwave part of the spectrum relies on radiation emitted by oxygen molecules at frequencies near 55 ghz. Calculate the wavelength and wavenumber of this radiation.
More informationATM S 111, Global Warming: Understanding the Forecast
ATM S 111, Global Warming: Understanding the Forecast DARGAN M. W. FRIERSON DEPARTMENT OF ATMOSPHERIC SCIENCES DAY 1: OCTOBER 1, 2015 Outline How exactly the Sun heats the Earth How strong? Important concept
More informationEnergy Pathways in Earth s Atmosphere
BRSP - 10 Page 1 Solar radiation reaching Earth s atmosphere includes a wide spectrum of wavelengths. In addition to visible light there is radiation of higher energy and shorter wavelength called ultraviolet
More information1. Theoretical background
1. Theoretical background We consider the energy budget at the soil surface (equation 1). Energy flux components absorbed or emitted by the soil surface are: net radiation, latent heat flux, sensible heat
More informationInfrared Spectroscopy: Theory
u Chapter 15 Infrared Spectroscopy: Theory An important tool of the organic chemist is Infrared Spectroscopy, or IR. IR spectra are acquired on a special instrument, called an IR spectrometer. IR is used
More informationwhere h = 6.62 10-34 J s
Electromagnetic Spectrum: Refer to Figure 12.1 Molecular Spectroscopy: Absorption of electromagnetic radiation: The absorptions and emissions of electromagnetic radiation are related molecular-level phenomena
More informationPTYS/ASTR 206 Section 2 Spring 2007 Homework #2 (Page 1/5) NAME: KEY
PTYS/ASTR 206 Section 2 Spring 2007 Homework #2 (Page 1/5) NAME: KEY Due Date: start of class 2/6/2007 5 pts extra credit if turned in before 9:00AM (early!) (To get the extra credit, the assignment must
More informationAfter a wave passes through a medium, how does the position of that medium compare to its original position?
Light Waves Test Question Bank Standard/Advanced Name: Question 1 (1 point) The electromagnetic waves with the highest frequencies are called A. radio waves. B. gamma rays. C. X-rays. D. visible light.
More informationElectromagnetic Radiation Energy that comes to us from the sun is transported in the form of waves known as electromagnetic energy.
Electromagnetic Radiation Energy that comes to us from the sun is transported in the form of waves known as electromagnetic energy. This combines electricity and magnetism such that setting up an electric
More informationMultiple Choice Identify the choice that best completes the statement or answers the question.
Test 2 f14 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. Carbon cycles through the Earth system. During photosynthesis, carbon is a. released from wood
More informationSpecific Intensity. I ν =
Specific Intensity Initial question: A number of active galactic nuclei display jets, that is, long, nearly linear, structures that can extend for hundreds of kiloparsecs. Many have two oppositely-directed
More informationMCQ - ENERGY and CLIMATE
1 MCQ - ENERGY and CLIMATE 1. The volume of a given mass of water at a temperature of T 1 is V 1. The volume increases to V 2 at temperature T 2. The coefficient of volume expansion of water may be calculated
More informationRADIATION (SOLAR) Introduction. Solar Spectrum and Solar Constant. Distribution of Solar Insolation at the Top of the Atmosphere
RADIATION (SOLAR) 1859 Workshop Proceedings, Joint Research Centre, Ispra, Italy, pp. 45 53. Ulaby FT (1981)Microwave response of vegetation. In Kahle AB, Weill G, Carter WD (eds) Advances in Space Research,
More informationFrom lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation?
From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation? From lowest energy to highest energy, which of the following correctly
More information- thus, the total number of atoms per second that absorb a photon is
Stimulated Emission of Radiation - stimulated emission is referring to the emission of radiation (a photon) from one quantum system at its transition frequency induced by the presence of other photons
More informationOverview of the IR channels and their applications
Ján Kaňák Slovak Hydrometeorological Institute Jan.kanak@shmu.sk Overview of the IR channels and their applications EUMeTrain, 14 June 2011 Ján Kaňák, SHMÚ 1 Basics in satellite Infrared image interpretation
More informationRESULTS FROM A SIMPLE INFRARED CLOUD DETECTOR
RESULTS FROM A SIMPLE INFRARED CLOUD DETECTOR A. Maghrabi 1 and R. Clay 2 1 Institute of Astronomical and Geophysical Research, King Abdulaziz City For Science and Technology, P.O. Box 6086 Riyadh 11442,
More information8.1 Radio Emission from Solar System objects
8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio
More informationThe Electromagnetic Spectrum
INTRODUCTION The Electromagnetic Spectrum I. What is electromagnetic radiation and the electromagnetic spectrum? What do light, X-rays, heat radiation, microwaves, radio waves, and gamma radiation have
More information-1- Electromagnetic radiation (EMR) basics for remote sensing
-1- Electromagnetic radiation (EMR) basics for remote sensing HANDOUT s OBJECTIVES: familiarize student with basic EMR terminology & mathematics overview of EMR polarization as related to remote sensing
More informationLet s consider a homogeneous medium characterized by the extinction coefficient β ext, single scattering albedo ω 0 and phase function P(µ, µ').
Lecture 22. Methods for solving the radiative transfer equation with multiple scattering. Part 4: Monte Carlo method. Radiative transfer methods for inhomogeneous ouds. Objectives: 1. Monte Carlo method.
More informationINSPIRE GK12 Lesson Plan. The Chemistry of Climate Change Length of Lesson
Lesson Title The Chemistry of Climate Change Length of Lesson 180 min Created By David Wilson Subject Physical Science / Chemistry / Organic Chemistry Grade Level 8-12 State Standards 2c, 4d / 2a, 4d /
More informationThe Greenhouse Effect. Lan Ma Global Warming: Problems & Solutions 17 September, 2007
The Greenhouse Effect Lan Ma Global Warming: Problems & Solutions 17 September, 2007 What to cover today: How do we calculate the Earth s surface temperature? What makes a gas a greenhouse gas and how
More informationHEAT AND MASS TRANSFER
MEL242 HEAT AND MASS TRANSFER Prabal Talukdar Associate Professor Department of Mechanical Engineering g IIT Delhi prabal@mech.iitd.ac.in MECH/IITD Course Coordinator: Dr. Prabal Talukdar Room No: III,
More informationThe Earth's Atmosphere. Layers of the Earth's Atmosphere
The Earth's Atmosphere The atmosphere surrounds Earth and protects us by blocking out dangerous rays from the sun. The atmosphere is a mixture of gases that becomes thinner until it gradually reaches space.
More informationWaves Sound and Light
Waves Sound and Light r2 c:\files\courses\1710\spr12\wavetrans.doc Ron Robertson The Nature of Waves Waves are a type of energy transmission that results from a periodic disturbance (vibration). They are
More informationClimate Change and Renewable Energy A Perspective from a Measurements Viewpoint
Climate Change and Renewable Energy A Perspective from a Measurements Viewpoint Regional Workshop on Metrology and Technology Challenges of Climate Change and Renewable Energy Guatemala City, Guatemala
More informationExamination Space Missions and Applications I (AE2103) Faculty of Aerospace Engineering Delft University of Technology SAMPLE EXAM
Examination Space Missions and Applications I AE2103 Faculty of Aerospace Engineering Delft University of Technology SAMPLE EXAM Please read these instructions first: This are a series of multiple-choice
More informationSemester 2. Final Exam Review
Semester 2 Final Exam Review Motion and Force Vocab Motion object changes position relative to a reference point. Speed distance traveled in a period of time. Velocity speed in a direction. Acceleration
More informationFor further information, and additional background on the American Meteorological Society s Education Program, please contact:
Project ATMOSPHERE This guide is one of a series produced by Project ATMOSPHERE, an initiative of the American Meteorological Society. Project ATMOSPHERE has created and trained a network of resource agents
More informationAstronomy 110 Homework #04 Assigned: 02/06/2007 Due: 02/13/2007. Name:
Astronomy 110 Homework #04 Assigned: 02/06/2007 Due: 02/13/2007 Name: Directions: Listed below are twenty (20) multiple-choice questions based on the material covered by the lectures this past week. Choose
More informationThe Fundamentals of Infrared Spectroscopy. Joe Van Gompel, PhD
TN-100 The Fundamentals of Infrared Spectroscopy The Principles of Infrared Spectroscopy Joe Van Gompel, PhD Spectroscopy is the study of the interaction of electromagnetic radiation with matter. The electromagnetic
More informationAS COMPETITION PAPER 2008
AS COMPETITION PAPER 28 Name School Town & County Total Mark/5 Time Allowed: One hour Attempt as many questions as you can. Write your answers on this question paper. Marks allocated for each question
More informationCloud Radiation and the Law of Attraction
Convec,on, cloud and radia,on Convection redistributes the thermal energy yielding (globally-averaged), a mean lapse rate of ~ -6.5 o C/km. Radiative processes tend to produce a more negative temperature
More informationAbsorption by atmospheric gases in the IR, visible and UV spectral regions.
Lecture 6. Absorption by atmospheric gases in the IR, visible and UV spectral regions. Objectives: 1. Gaseous absorption in thermal IR. 2. Gaseous absorption in the visible and near infrared. 3. Gaseous
More informationRate Equations and Detailed Balance
Rate Equations and Detailed Balance Initial question: Last time we mentioned astrophysical masers. Why can they exist spontaneously? Could there be astrophysical lasers, i.e., ones that emit in the optical?
More informationWaves - Transverse and Longitudinal Waves
Waves - Transverse and Longitudinal Waves wave may be defined as a periodic disturbance in a medium that carries energy from one point to another. ll waves require a source and a medium of propagation.
More informationIntroduction to the Greenhouse Effect
Introduction to the Greenhouse Effect Planetary Temperature by Arthur Glasfeld and Margret Geselbracht ver the past 10-15 years there has been growing concern over changes in the climate and the possibility
More informationApplication Note AN4
TAKING INVENTIVE STEPS IN INFRARED. MINIATURE INFRARED GAS SENSORS GOLD SERIES UK Patent App. No. 2372099A USA Patent App. No. 09/783,711 World Patents Pending INFRARED SPECTROSCOPY Application Note AN4
More informationCopyrighted Material. 1 Basics of Climate. The climate s delicate, the air most sweet. William Shakespeare, A Winter s Tale
1 Basics of Climate The climate s delicate, the air most sweet. William Shakespeare, A Winter s Tale To appreciate the role of the ocean in climate, we need to have a basic understanding of how the climate
More informationThe Role of Electric Polarization in Nonlinear optics
The Role of Electric Polarization in Nonlinear optics Sumith Doluweera Department of Physics University of Cincinnati Cincinnati, Ohio 45221 Abstract Nonlinear optics became a very active field of research
More informationEnergy. Mechanical Energy
Principles of Imaging Science I (RAD119) Electromagnetic Radiation Energy Definition of energy Ability to do work Physicist s definition of work Work = force x distance Force acting upon object over distance
More informationSOLAR ENERGY How much strikes the earth? How much can my building get? When is it too much?
SOLAR ENERGY How much strikes the earth? How much can my building get? When is it too much? The sun: friend of foe? Drawing by Le Corbusier ENGS 44 Sustainable Design Benoit Cushman-Roisin 14 April 2015
More informationESCI-61 Introduction to Photovoltaic Technology. Solar Radiation. Ridha Hamidi, Ph.D.
1 ESCI-61 Introduction to Photovoltaic Technology Solar Radiation Ridha Hamidi, Ph.D. 2 The Sun The Sun is a perpetual source of energy It has produced energy for about 4.6 billions of years, and it is
More informationThe Three Heat Transfer Modes in Reflow Soldering
Section 5: Reflow Oven Heat Transfer The Three Heat Transfer Modes in Reflow Soldering There are three different heating modes involved with most SMT reflow processes: conduction, convection, and infrared
More informationEarth Sciences -- Grades 9, 10, 11, and 12. California State Science Content Standards. Mobile Climate Science Labs
Earth Sciences -- Grades 9, 10, 11, and 12 California State Science Content Standards Covered in: Hands-on science labs, demonstrations, & activities. Investigation and Experimentation. Lesson Plans. Presented
More informationTotal radiative heating/cooling rates.
Lecture. Total radiative heating/cooling rates. Objectives:. Solar heating rates.. Total radiative heating/cooling rates in a cloudy atmosphere.. Total radiative heating/cooling rates in different aerosol-laden
More informationATMOSPHERIC STRUCTURE. The vertical distribution of temperature, pressure,
ATMOSPHERIC STRUCTURE. The vertical distribution of temperature, pressure, density, and composition of the atmosphere constitutes atmospheric structure. These quantities also vary with season and location
More informationThe atmospheres of different planets
The atmospheres of different planets Thomas Baron October 13, 2006 1 Contents 1 Introduction 3 2 The atmosphere of the Earth 3 2.1 Description and Composition.................... 3 2.2 Discussion...............................
More informationLecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
More informationExperiment #5: Qualitative Absorption Spectroscopy
Experiment #5: Qualitative Absorption Spectroscopy One of the most important areas in the field of analytical chemistry is that of spectroscopy. In general terms, spectroscopy deals with the interactions
More informationAntennas & Propagation. CS 6710 Spring 2010 Rajmohan Rajaraman
Antennas & Propagation CS 6710 Spring 2010 Rajmohan Rajaraman Introduction An antenna is an electrical conductor or system of conductors o Transmission - radiates electromagnetic energy into space o Reception
More information7. Our Solar System. Planetary Orbits to Scale. The Eight Planetary Orbits
7. Our Solar System Terrestrial & Jovian planets Seven large satellites [moons] Chemical composition of the planets Asteroids & comets The Terrestrial & Jovian Planets Four small terrestrial planets Like
More informationCHAPTER 6 THE TERRESTRIAL PLANETS
CHAPTER 6 THE TERRESTRIAL PLANETS MULTIPLE CHOICE 1. Which of the following is NOT one of the four stages in the development of a terrestrial planet? 2. That Earth, evidence that Earth differentiated.
More informationThe Sun. Solar radiation (Sun Earth-Relationships) The Sun. The Sun. Our Sun
The Sun Solar Factoids (I) The sun, a medium-size star in the milky way galaxy, consisting of about 300 billion stars. (Sun Earth-Relationships) A gaseous sphere of radius about 695 500 km (about 109 times
More informationTrace Gas Exchange Measurements with Standard Infrared Analyzers
Practical Environmental Measurement Methods Trace Gas Exchange Measurements with Standard Infrared Analyzers Last change of document: February 23, 2007 Supervisor: Charles Robert Room no: S 4381 ph: 4352
More informationLight Waves and Matter
Name: Light Waves and Matter Read from Lesson 2 of the Light Waves and Color chapter at The Physics Classroom: http://www.physicsclassroom.com/class/light/u12l2a.html MOP Connection: Light and Color: sublevel
More informationRaman spectroscopy Lecture
Raman spectroscopy Lecture Licentiate course in measurement science and technology Spring 2008 10.04.2008 Antti Kivioja Contents - Introduction - What is Raman spectroscopy? - The theory of Raman spectroscopy
More informationEnergy Transport. Focus on heat transfer. Heat Transfer Mechanisms: Conduction Radiation Convection (mass movement of fluids)
Energy Transport Focus on heat transfer Heat Transfer Mechanisms: Conduction Radiation Convection (mass movement of fluids) Conduction Conduction heat transfer occurs only when there is physical contact
More informationName Class Date. spectrum. White is not a color, but is a combination of all colors. Black is not a color; it is the absence of all light.
Exercises 28.1 The Spectrum (pages 555 556) 1. Isaac Newton was the first person to do a systematic study of color. 2. Circle the letter of each statement that is true about Newton s study of color. a.
More informationPreview of Period 3: Electromagnetic Waves Radiant Energy II
Preview of Period 3: Electromagnetic Waves Radiant Energy II 3.1 Radiant Energy from the Sun How is light reflected and transmitted? What is polarized light? 3.2 Energy Transfer with Radiant Energy How
More informationCommon Defects in Digital Printing. Paul Geldenhuys & Amir Shapira January, 2009
Common Defects in Digital Printing Paul Geldenhuys & Amir Shapira January, 2009 Overview Ambient Influences Humidity Temperature Sunlight & UV Abrasion Chemical Resistance Common Defects in Digital Printing
More informationCalifornia Standards Grades 9 12 Boardworks 2009 Science Contents Standards Mapping
California Standards Grades 912 Boardworks 2009 Science Contents Standards Mapping Earth Sciences Earth s Place in the Universe 1. Astronomy and planetary exploration reveal the solar system s structure,
More informationPHOTOELECTRIC EFFECT AND DUAL NATURE OF MATTER AND RADIATIONS
PHOTOELECTRIC EFFECT AND DUAL NATURE OF MATTER AND RADIATIONS 1. Photons 2. Photoelectric Effect 3. Experimental Set-up to study Photoelectric Effect 4. Effect of Intensity, Frequency, Potential on P.E.
More informationPhysics 9e/Cutnell. correlated to the. College Board AP Physics 1 Course Objectives
Physics 9e/Cutnell correlated to the College Board AP Physics 1 Course Objectives Big Idea 1: Objects and systems have properties such as mass and charge. Systems may have internal structure. Enduring
More informationEvaluation of the Effect of Upper-Level Cirrus Clouds on Satellite Retrievals of Low-Level Cloud Droplet Effective Radius
Evaluation of the Effect of Upper-Level Cirrus Clouds on Satellite Retrievals of Low-Level Cloud Droplet Effective Radius F.-L. Chang and Z. Li Earth System Science Interdisciplinary Center University
More informationChapter 18 Temperature, Heat, and the First Law of Thermodynamics. Problems: 8, 11, 13, 17, 21, 27, 29, 37, 39, 41, 47, 51, 57
Chapter 18 Temperature, Heat, and the First Law of Thermodynamics Problems: 8, 11, 13, 17, 21, 27, 29, 37, 39, 41, 47, 51, 57 Thermodynamics study and application of thermal energy temperature quantity
More informationModule 2.2. Heat transfer mechanisms
Module 2.2 Heat transfer mechanisms Learning Outcomes On successful completion of this module learners will be able to - Describe the 1 st and 2 nd laws of thermodynamics. - Describe heat transfer mechanisms.
More informationHow To Understand The Physics Of Electromagnetic Radiation
Ay 122 - Fall 2004 Electromagnetic Radiation And Its Interactions With Matter (This version has many of the figures missing, in order to keep the pdf file reasonably small) Radiation Processes: An Overview
More informationLectures Remote Sensing
Lectures Remote Sensing ATMOSPHERIC CORRECTION dr.ir. Jan Clevers Centre of Geo-Information Environmental Sciences Wageningen UR Atmospheric Correction of Optical RS Data Background When needed? Model
More informationComposition of the Atmosphere. Outline Atmospheric Composition Nitrogen and Oxygen Lightning Homework
Molecules of the Atmosphere The present atmosphere consists mainly of molecular nitrogen (N2) and molecular oxygen (O2) but it has dramatically changed in composition from the beginning of the solar system.
More information