Key Concepts and Fundamental Theorems of Atmospheric Science
|
|
- Kelly Clark
- 5 years ago
- Views:
Transcription
1 Key Concepts and Fundamental Theorems of Atmospheric Science Part I Global Thermodynamics John A. Dutton Meteo 485 Spring 2004
2 Goals and strategy Because skillful prediction requires understanding, we will try to Clarify links between cause and effect in large-scale atmospheric flow Illustrate how theory uses observations to create models and reach conclusions Inquire why the atmosphere behaves as it does Why are things the way they are?
3 Geometry of the Planet Area of a circle 2π r dr dθ = π R 2 0 R 0 r θ Surface area of a sphere π R 2 2π 2 0 π 2 cosϕ dϕ dλ = 4π R 2 R cosϕ ϕ
4
5 Let there be light Sunlight of intensity I 0 falls on a disc of area πr 2 Earth emits radiation F = σt 4 as a sphere of area 4πR 2 F = σt 4 = I o / 4 I 0 = 1360 W/m 2, σ = W/m 2 K 4 ==> T 0 ~ 278 K Planetary albedo α = 0.32 J = (1 - α) I 0 /4 = (J/ σ) 1/4-273 = C
6 Let there be warmth Average surface temperature T s = K compared to T α = 253 K implies there must be another flux of energy G F s = σt s 4 = J + G µ = G/F s = (F s - J)/F s = J µf s F s (1-µ) F s
7 Let there be latitudinal variation α(ϕ)= a Global Albedo Global Albedo +b cos(ϕ / 2) a = b = Albedo (per cent) Approximation Observed Latitude α = π 2 α(ϕ)cos(ϕ)dϕ =
8
9 Zenith Angles cos Z = sin ϕ sin δ + cos ϕ cos δ cos h at equinox, δ = 0; at sunrise and sunset, h = π/2 Z cos Z = cos ϕ cos h Averaging along a latitude circle 1 2π π /2 cos(h) dh = 1 π /2 π J(ϕ) = 1 π (1 α(ϕ))i 0 cos(ϕ)
10 Surface temperature estimate F = J + G = J + µf T s (ϕ) = [J(ϕ)/σ(1- µ)] 1/4 Surface Temperature (C) Latitude
11 Zonal Average Sea Surface Temperature Observation Temperature (C) Approximation Latitude aa=28.72 bb=0.564 Tocn = aa cos2(ϕ)/(1+bb ϕ2) Focn = σ Tocn4(ϕ) 100
12 Solar and Longwave Radiation 400 Solar J(ϕ) Watts/m^ Longwave F ocn (1-µ) Latitude
13 Solar and Longwave Radiation 400 Solar J(ϕ) 300 Watts/m^2 200 Longwave F ocn / (1-µ) Sin(Latitude)
14 Balancing the energy flow Poleward Heat Flux H(ϕ) = F ocean (ϕ)(1 µ) J(ϕ) 30 H p (ϕ) = ϕ π 2 H(ψ )cos(ψ )dψ H(ϕ) = F ocean (ϕ)(1 µ) J(ϕ) Heat Flux (W/m^2) H p (ϕ) = π 2 ϕ H(ψ )cos(ψ )dψ Latitude
15 Balancing the energy flow Solve for the µ that balances the energy flow H(ϕ) = F ocean (ϕ)(1 µ) J(ϕ) µ = 0 π 2 (F ocean (ϕ) J(ϕ))cos(ϕ)dϕ 0 π 2 F ocean (ϕ)cos(ϕ)dϕ = 0.412
16 Poleward Heat Flux 30 Heat Flux (W/m^2) Latitude
17 Latitudinal Heat Flux Estimates Houghton (1954) Oort & Vonder Haar (1976) Present Model (mu=0.399) Present Model (mu=0.411) Heat Flux (W/m^2) Latitude
18 So what do the thermodynamic gods ordain that the atmosphere and ocean must do? Transfer heat from the equator toward the poles, forevermore. As long as the Earth is round, the wind may never cease.
19 Let us turn this inescapable but qualitative conclusion into a definite statement a theorem, if you will.
20 T t c V ρ dt ρ t The Equations of Atmospheric Motion No motion: v(x,t) = v t = 0 x, t = t 0 dv dt = 1 ρ p gk 2Ω v + 1 µ v +... ρ dt + p v = R + k T + C+ v dρ dt + ρ v = 0 p = ρrt dq dt + q v = S + k q q d(g) dt = (g) t + v (g) q = C = 0
21 The Motionless State p = gρk z p = 0, p z z = p z z = g z ρ = 0 p z = gρ z p = Rρ z T + RT z ρ T z = 0 for Q = R, z Q = 0
22 The First Fundamental Theorem of Atmospheric Science If no motion z T = 0, then z T 0 motion. Theorem (Jeffreys, 1925) As long as there are horizontal variations in heating (or equivalently, temperature), then the atmosphere must remain in motion in the sense that the velocity and acceleration cannot both vanish identically.
23 But if the thermodynamic gods ordain that the atmosphere and ocean transfer heat from the equator toward the poles, why are there westerlies instead of northerlies or southerlies? Because the Earth rotates and the poleward temperature gradients are large.
24 why do the westerlies increase with height?
25 For Ro = V fl ~ 10 1 Re = VL υ ~ and slowly-varying flows,... and then v H v g = 1 ρ f k z p v g z g ft k z T v g p = R fp k p T v g θ = c p f θ k θ T
26 why do the westerlies increase with height? Because it is colder toward the poles and that s because the Earth is round.
Friday 8 September, :00-4:00 Class#05
Friday 8 September, 2017 3:00-4:00 Class#05 Topics for the hour Global Energy Budget, schematic view Solar Radiation Blackbody Radiation http://www2.gi.alaska.edu/~bhatt/teaching/atm694.fall2017/ notes.html
More information2. Meridional atmospheric structure; heat and water transport. Recall that the most primitive equilibrium climate model can be written
2. Meridional atmospheric structure; heat and water transport The equator-to-pole temperature difference DT was stronger during the last glacial maximum, with polar temperatures down by at least twice
More informationLecture 3. Background materials. Planetary radiative equilibrium TOA outgoing radiation = TOA incoming radiation Figure 3.1
Lecture 3. Changes in planetary albedo. Is there a clear signal caused by aerosols and clouds? Outline: 1. Background materials. 2. Papers for class discussion: Palle et al., Changes in Earth s reflectance
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 informationGoverning Equations and Scaling in the Tropics
Governing Equations and Scaling in the Tropics M 1 ( ) e R ε er Tropical v Midlatitude Meteorology Why is the general circulation and synoptic weather systems in the tropics different to the those in the
More informationMeteorology 6150 Cloud System Modeling
Meteorology 6150 Cloud System Modeling Steve Krueger Spring 2009 1 Fundamental Equations 1.1 The Basic Equations 1.1.1 Equation of motion The movement of air in the atmosphere is governed by Newton s Second
More informationLecture 1b: Global Energy Balance. Instructor: Prof. Johnny Luo
Lecture 1b: Global Energy Balance Instructor: Prof. Johnny Luo Daily average insola>on A few points: 1. Solar constant ~ 1361 W m -2. But averaged over a whole day, we get much less. 2. At NYC in Jan,
More informationLecture 11: Meridonal structure of the atmosphere
Lecture 11: Meridonal structure of the atmosphere September 28, 2003 1 Meridional structure of the atmosphere In previous lectures we have focussed on the vertical structure of the atmosphere. Today, we
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 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 informationLecture 2: Light And Air
Lecture 2: Light And Air Earth s Climate System Earth, Mars, and Venus Compared Solar Radiation Greenhouse Effect Thermal Structure of the Atmosphere Atmosphere Ocean Solid Earth Solar forcing Land Energy,
More informationIntroduction to Atmospheric Circulation
Introduction to Atmospheric Circulation Start rotating table Start heated bottle experiment Scientific Practice Observe nature Develop a model*/hypothesis for what is happening Carry out experiments Make
More informationLecture 3: Global Energy Cycle
Lecture 3: Global Energy Cycle Planetary energy balance Greenhouse Effect Vertical energy balance Latitudinal energy balance Seasonal and diurnal cycles Solar Flux and Flux Density Solar Luminosity (L)
More informationThe Energy Balance Model
1 The Energy Balance Model 2 D.S. Battisti 3 Dept. of Atmospheric Sciences, University of Washington, Seattle Generated using v.3.2 of the AMS LATEX template 1 ABSTRACT 5 ad 2 6 1. Zero-order climatological
More informationAtmospheric Circulation
Atmospheric Circulation (WAPE: General Circulation of the Atmosphere and Variability) François Lott, flott@lmd.ens.fr http://web.lmd.jussieu.fr/~flott 1) Mean climatologies and equations of motion a)thermal,
More informationIntegrals in cylindrical, spherical coordinates (Sect. 15.7)
Integrals in clindrical, spherical coordinates (Sect. 15.7 Integration in spherical coordinates. Review: Clindrical coordinates. Spherical coordinates in space. Triple integral in spherical coordinates.
More informationTorben Königk Rossby Centre/ SMHI
Fundamentals of Climate Modelling Torben Königk Rossby Centre/ SMHI Outline Introduction Why do we need models? Basic processes Radiation Atmospheric/Oceanic circulation Model basics Resolution Parameterizations
More informationIntroduction to Atmospheric Circulation
Introduction to Atmospheric Circulation Start rotating table Cloud Fraction Dice Results from http://eos.atmos.washington.edu/erbe/ from http://eos.atmos.washington.edu/erbe/ from http://eos.atmos.washington.edu/erbe/
More informationDynamics of the Zonal-Mean, Time-Mean Tropical Circulation
Dynamics of the Zonal-Mean, Time-Mean Tropical Circulation First consider a hypothetical planet like Earth, but with no continents and no seasons and for which the only friction acting on the atmosphere
More information1. The vertical structure of the atmosphere. Temperature profile.
Lecture 4. The structure of the atmosphere. Air in motion. Objectives: 1. The vertical structure of the atmosphere. Temperature profile. 2. Temperature in the lower atmosphere: dry adiabatic lapse rate.
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 informationLecture 2: Global Energy Cycle
Lecture 2: Global Energy Cycle Planetary energy balance Greenhouse Effect Vertical energy balance Solar Flux and Flux Density Solar Luminosity (L) the constant flux of energy put out by the sun L = 3.9
More informationATMS 321: Sci. of Climate Final Examination Study Guide Page 1 of 4
ATMS 321: Sci. of Climate Final Examination Study Guide Page 1 of 4 Atmospheric Sciences 321: Final Examination Study Guide The final examination will consist of similar questions Science of Climate Multiple
More informationEarth Systems Science Chapter 3
Earth Systems Science Chapter 3 ELECTROMAGNETIC RADIATION: WAVES I. Global Energy Balance and the Greenhouse Effect: The Physics of the Radiation Balance of the Earth 1. Electromagnetic Radiation: waves,
More informationDynamics and Kinematics
Geophysics Fluid Dynamics () Syllabus Course Time Lectures: Tu, Th 09:30-10:50 Discussion: 3315 Croul Hall Text Book J. R. Holton, "An introduction to Dynamic Meteorology", Academic Press (Ch. 1, 2, 3,
More informationSIO 210 Introduction to Physical Oceanography Mid-term examination November 3, 2014; 1 hour 20 minutes
NAME: SIO 210 Introduction to Physical Oceanography Mid-term examination November 3, 2014; 1 hour 20 minutes Closed book; one sheet of your own notes is allowed. A calculator is allowed. (100 total points.)
More information14.1 Simple model of global radiation balance
Chapter 1 Global Circulations 1.1 Simple model of global radiation balance The earth receives energy from the sun in the form of visible, near-infrared, and ultraviolet radiation. Most of this energy is
More informationChapter 1. Governing Equations of GFD. 1.1 Mass continuity
Chapter 1 Governing Equations of GFD The fluid dynamical governing equations consist of an equation for mass continuity, one for the momentum budget, and one or more additional equations to account for
More informationGeophysics Fluid Dynamics (ESS228)
Geophysics Fluid Dynamics (ESS228) Course Time Lectures: Tu, Th 09:30-10:50 Discussion: 3315 Croul Hall Text Book J. R. Holton, "An introduction to Dynamic Meteorology", Academic Press (Ch. 1, 2, 3, 4,
More informationElectromagnetic Radiation. Radiation and the Planetary Energy Balance. Electromagnetic Spectrum of the Sun
Radiation and the Planetary Energy Balance Electromagnetic Radiation Solar radiation warms the planet Conversion of solar energy at the surface Absorption and emission by the atmosphere The greenhouse
More informationEART164: PLANETARY ATMOSPHERES
EART164: PLANETARY ATMOSPHERES Francis Nimmo Last Week Radiative Transfer Black body radiation, Planck function, Wien s law Absorption, emission, opacity, optical depth Intensity, flux Radiative diffusion,
More informationSolar Insolation and Earth Radiation Budget Measurements
Week 13: November 19-23 Solar Insolation and Earth Radiation Budget Measurements Topics: 1. Daily solar insolation calculations 2. Orbital variations effect on insolation 3. Total solar irradiance measurements
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 informationATMS 321 Problem Set 1 30 March 2012 due Friday 6 April. 1. Using the radii of Earth and Sun, calculate the ratio of Sun s volume to Earth s volume.
ATMS 321 Problem Set 1 30 March 2012 due Friday 6 April 1. Using the radii of Earth and Sun, calculate the ratio of Sun s volume to Earth s volume. 2. The Earth-Sun distance varies from its mean by ±1.75%
More informationReynolds Averaging. We separate the dynamical fields into slowly varying mean fields and rapidly varying turbulent components.
Reynolds Averaging Reynolds Averaging We separate the dynamical fields into sloly varying mean fields and rapidly varying turbulent components. Reynolds Averaging We separate the dynamical fields into
More informationImperial College London
Solar Influence on Stratosphere-Troposphere Dynamical Coupling Isla Simpson, Joanna D. Haigh, Space and Atmospheric Physics, Imperial College London Mike Blackburn, Department of Meteorology, University
More informationTopic # 12 HOW CLIMATE WORKS
Topic # 12 HOW CLIMATE WORKS A Primer on How the Energy Balance Drives Atmospheric & Oceanic Circulation, Natural Climatic Processes Starts on p 67 in Class Notes Evidently, not scary enough. How do we
More informationLecture 6. Solar vs. terrestrial radiation and the bare rock climate model.
Lecture 6 Solar vs. terrestrial radiation and the bare rock climate model. Radiation Controls energy balance of Earth Is all around us all the time. Can be labeled by its source (solar, terrestrial) or
More informationGlobal Energy Balance. GEOG/ENST 2331: Lecture 4 Ahrens: Chapter 2
Global Energy Balance GEOG/ENST 2331: Lecture 4 Ahrens: Chapter 2 Solstices and Equinoxes Winter Solstice was on December 21 last year 8 hours 22 minutes of daylight March (Vernal) Equinox: March 20 this
More informationLecture 4: Global Energy Balance
Lecture : Global Energy Balance S/ * (1-A) T A T S T A Blackbody Radiation Layer Model Greenhouse Effect Global Energy Balance terrestrial radiation cooling Solar radiation warming Global Temperature atmosphere
More information2. Conservation laws and basic equations
2. Conservation laws and basic equations Equatorial region is mapped well by cylindrical (Mercator) projection: eastward, northward, upward (local Cartesian) coordinates:,, velocity vector:,,,, material
More informationLecture 4: Global Energy Balance. Global Energy Balance. Solar Flux and Flux Density. Blackbody Radiation Layer Model.
Lecture : Global Energy Balance Global Energy Balance S/ * (1-A) terrestrial radiation cooling Solar radiation warming T S Global Temperature Blackbody Radiation ocean land Layer Model energy, water, and
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 informationMAPH & & & & & & 02 LECTURE
Climate & Earth System Science Introduction to Meteorology & Climate MAPH 10050 Peter Lynch Peter Lynch Meteorology & Climate Centre School of Mathematical Sciences University College Dublin Meteorology
More informationThe Arctic Energy Budget
The Arctic Energy Budget The global heat engine [courtesy Kevin Trenberth, NCAR]. Differential solar heating between low and high latitudes gives rise to a circulation of the atmosphere and ocean that
More informationMAE 101A. Homework 7 - Solutions 3/12/2018
MAE 101A Homework 7 - Solutions 3/12/2018 Munson 6.31: The stream function for a two-dimensional, nonviscous, incompressible flow field is given by the expression ψ = 2(x y) where the stream function has
More informationTopic # 12 How Climate Works
Topic # 12 How Climate Works A Primer on How the Energy Balance Drives Atmospheric & Oceanic Circulation, Natural Climatic Processes pp 63-68 in Class Notes How do we get energy from this........ to drive
More informationLecture 4: Heat, and Radiation
Lecture 4: Heat, and Radiation Heat Heat is a transfer of energy from one object to another. Heat makes things warmer. Heat is measured in units called calories. A calorie is the heat (energy) required
More informationESCI 485 Air/Sea Interaction Lesson 1 Stresses and Fluxes Dr. DeCaria
ESCI 485 Air/Sea Interaction Lesson 1 Stresses and Fluxes Dr DeCaria References: An Introduction to Dynamic Meteorology, Holton MOMENTUM EQUATIONS The momentum equations governing the ocean or atmosphere
More informationChapter 5. Shallow Water Equations. 5.1 Derivation of shallow water equations
Chapter 5 Shallow Water Equations So far we have concentrated on the dynamics of small-scale disturbances in the atmosphere and ocean with relatively simple background flows. In these analyses we have
More informationAT622 Section 5 The Sun
AT622 Section 5 The Sun The main aim here is to acquaint the student with basic radiative properties of the sun and the factors that govern the disposition of solar radiation received at Earth. 5.1 The
More informationLecture 3a: Surface Energy Balance
Lecture 3a: Surface Energy Balance Instructor: Prof. Johnny Luo http://www.sci.ccny.cuny.edu/~luo Surface Energy Balance 1. Factors affecting surface energy balance 2. Surface heat storage 3. Surface
More informationSunlight and its Properties Part I. EE 446/646 Y. Baghzouz
Sunlight and its Properties Part I EE 446/646 Y. Baghzouz The Sun a Thermonuclear Furnace The sun is a hot sphere of gas whose internal temperatures reach over 20 million deg. K. Nuclear fusion reaction
More information4-1 The Role of Climate
4-1 The Role of Climate 1 of 26 What Is Climate? What Is Climate? Weather is the day-to-day condition of Earth's atmosphere at a particular time and place. Climate refers to the average year-after-year
More information4-1 The Role of Climate
biology 1 of 26 2 of 26 What Is Climate? What Is Climate? Weather is the day-to-day condition of Earth's atmosphere at a particular time and place. Climate refers to the average year-after-year conditions
More informationMath Exam IV - Fall 2011
Math 233 - Exam IV - Fall 2011 December 15, 2011 - Renato Feres NAME: STUDENT ID NUMBER: General instructions: This exam has 16 questions, each worth the same amount. Check that no pages are missing and
More information4. Zero-dimensional Model of Earth s Temperature
4. Zero-dimensional Model of Earth s Temperature Introduction The term zero-dimensional implies that the earth is treated as a single point having a single temperature. Later we will consider a one-dimensional
More informationTopic # 12 Natural Climate Processes
Topic # 12 Natural Climate Processes A Primer on How the Energy Balance Drives Atmospheric & Oceanic Circulation, Natural Climatic Processes pp 63-68 in Class Notes RADIATION / ENERGY BALANCE Radiation
More informationInsolation and Temperature variation. The Sun & Insolation. The Sun (cont.) The Sun
Insolation and Temperature variation Atmosphere: blanket of air surrounding earth Without our atmosphere: cold, quiet, cratered place Dynamic: currents and circulation cells June 23, 2008 Atmosphere important
More information(after Stephens et al. 2012)
Energy Balance Incoming solar radiation 34 Reflected solar radiation Outgoing longwave radiation 1 24 TOA 75 Atmospheric absorption Atmospheric reflection 77 Atmospheric window 4 165 35 Clear Sky Cloud
More informationMeteorology 311. General Circulation/Fronts Fall 2017
Meteorology 311 General Circulation/Fronts Fall 2017 Precipitation Types Rain Snow growth of ice crystals through deposition, accretion, and aggregation. Freezing Rain Rain freezes when it hits the surface.
More information1) The energy balance at the TOA is: 4 (1 α) = σt (1 0.3) = ( ) 4. (1 α) 4σ = ( S 0 = 255 T 1
EAS488/B8800 Climate & Climate Change Homework 2: Atmospheric Radiation and Climate, surface energy balance, and atmospheric general circulation Posted: 3/12/18; due: 3/26/18 Answer keys 1. (10 points)
More informationOverview of fundamental atmospheric concepts
Fundamentals of Earth s Atmosphere AOSC 433/633 & CHEM 433/633 Tim Canty Class Web Site: http://www.atmos.umd.edu/~rjs/class/spr2013 Notes: Ross, Tim, & Allison co-teach this class; please include all
More informationChapter 7: Thermodynamics
Chapter 7: Thermodynamics 7.1 Sea surface heat budget In Chapter 5, we have introduced the oceanic planetary boundary layer-the Ekman layer. The observed T and S in this layer are almost uniform vertically,
More information( u,v). For simplicity, the density is considered to be a constant, denoted by ρ 0
! Revised Friday, April 19, 2013! 1 Inertial Stability and Instability David Randall Introduction Inertial stability and instability are relevant to the atmosphere and ocean, and also in other contexts
More informationChapter 2. Quasi-Geostrophic Theory: Formulation (review) ε =U f o L <<1, β = 2Ω cosθ o R. 2.1 Introduction
Chapter 2. Quasi-Geostrophic Theory: Formulation (review) 2.1 Introduction For most of the course we will be concerned with instabilities that an be analyzed by the quasi-geostrophic equations. These are
More informationLecture 2: Global Energy Cycle
Lecture 2: Global Energy Cycle Planetary energy balance Greenhouse Effect Selective absorption Vertical energy balance Solar Flux and Flux Density Solar Luminosity (L) the constant flux of energy put out
More informationSolar Flux and Flux Density. Lecture 2: Global Energy Cycle. Solar Energy Incident On the Earth. Solar Flux Density Reaching Earth
Lecture 2: Global Energy Cycle Solar Flux and Flux Density Planetary energy balance Greenhouse Effect Selective absorption Vertical energy balance Solar Luminosity (L) the constant flux of energy put out
More informationThe atmosphere: A general introduction Niels Woetmann Nielsen Danish Meteorological Institute
The atmosphere: A general introduction Niels Woetmann Nielsen Danish Meteorological Institute Facts about the atmosphere The atmosphere is kept in place on Earth by gravity The Earth-Atmosphere system
More informationHEATING THE ATMOSPHERE
HEATING THE ATMOSPHERE Earth and Sun 99.9% of Earth s heat comes from Sun But
More informationAtmosphere, Ocean and Climate Dynamics Answers to Chapter 8
Atmosphere, Ocean and Climate Dynamics Answers to Chapter 8 1. Consider a zonally symmetric circulation (i.e., one with no longitudinal variations) in the atmosphere. In the inviscid upper troposphere,
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 informationAtmospheric Thermodynamics
Atmospheric Thermodynamics Atmospheric Composition What is the composition of the Earth s atmosphere? Gaseous Constituents of the Earth s atmosphere (dry air) Constituent Molecular Weight Fractional Concentration
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 informationSpherical Shallow Water Turbulence: Cyclone-Anticyclone Asymmetry, Potential Vorticity Homogenisation and Jet Formation
Spherical Shallow Water Turbulence: Cyclone-Anticyclone Asymmetry, Potential Vorticity Homogenisation and Jet Formation Jemma Shipton Department of Atmospheric, Oceanic and Planetary Physics, University
More informationFundamentals of Earth s Atmosphere. AOSC 434/658R & CHEM 434/678A Tim Canty
Fundamentals of Earth s Atmosphere AOSC 434/658R & CHEM 434/678A Tim Canty Class Web Site: http://www.atmos.umd.edu/~rjs/class/spr2011 Notes: Please include both Ross and Tim on any class related email
More informationData and formulas at the end. Exam would be Weds. May 8, 2008
ATMS 321: Science of Climate Practice Mid Term Exam - Spring 2008 page 1 Atmospheric Sciences 321 Science of Climate Practice Mid-Term Examination: Would be Closed Book Data and formulas at the end. Exam
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 information4-1 The Role of Climate. Copyright Pearson Prentice Hall
4-1 The Role of Climate Copyright Pearson Prentice Hall What Is Climate? Weather is the day-to-day condition of Earth's atmosphere at a particular time and place. Climate refers to the average year-after-year
More informationLecture 9: Climate Sensitivity and Feedback Mechanisms
Lecture 9: Climate Sensitivity and Feedback Mechanisms Basic radiative feedbacks (Plank, Water Vapor, Lapse-Rate Feedbacks) Ice albedo & Vegetation-Climate feedback Cloud feedback Biogeochemical feedbacks
More informationATMOSPHERIC ENERGY and GLOBAL TEMPERATURES. Physical Geography (Geog. 300) Prof. Hugh Howard American River College
ATMOSPHERIC ENERGY and GLOBAL TEMPERATURES Physical Geography (Geog. 300) Prof. Hugh Howard American River College RADIATION FROM the SUN SOLAR RADIATION Primarily shortwave (UV-SIR) Insolation Incoming
More informationDynamic Meteorology - Introduction
Dynamic Meteorology - Introduction Atmospheric dynamics the study of atmospheric motions that are associated with weather and climate We will consider the atmosphere to be a continuous fluid medium, or
More informationHonour School of Physics Part C: 4 Year Course. Honour School of Physics and Philosophy Part C C5: PHYSICS OF ATMOSPHERES AND OCEANS TRINITY TERM 2016
A11048W1 SECOND PUBLIC EXAMINATION Honour School of Physics Part C: 4 Year Course Honour School of Physics and Philosophy Part C C5: PHYSICS OF ATMOSPHERES AND OCEANS TRINITY TERM 2016 Tuesday, 14 June,
More informationProblem 1, Lorentz transformations of electric and magnetic
Problem 1, Lorentz transformations of electric and magnetic fields We have that where, F µν = F µ ν = L µ µ Lν ν F µν, 0 B 3 B 2 ie 1 B 3 0 B 1 ie 2 B 2 B 1 0 ie 3 ie 2 ie 2 ie 3 0. Note that we use the
More informationAppearance of the Sky Orientation Motion of sky Seasons Precession (?)
Today Appearance of the Sky Orientation Motion of sky Seasons Precession (?) The Celestial Sphere Stars at different distances all appear to lie on the celestial sphere. The ecliptic is the Sun s apparent
More informationSolar radiation / radiative transfer
Solar radiation / radiative transfer The sun as a source of energy The sun is the main source of energy for the climate system, exceeding the next importat source (geothermal energy) by 4 orders of magnitude!
More informationMath 210, Final Exam, Spring 2012 Problem 1 Solution. (a) Find an equation of the plane passing through the tips of u, v, and w.
Math, Final Exam, Spring Problem Solution. Consider three position vectors (tails are the origin): u,, v 4,, w,, (a) Find an equation of the plane passing through the tips of u, v, and w. (b) Find an equation
More information- global radiative energy balance
(1 of 14) Further Reading: Chapter 04 of the text book Outline - global radiative energy balance - insolation and climatic regimes - composition of the atmosphere (2 of 14) Introduction Last time we discussed
More information1/55. Solar energy. solar radiation definitions incident solar energy
1/55 Solar energy solar radiation definitions incident solar energy 2/55 Sun closest star centre of our planetary system solar system 3/55 Sun diameter 1 392 000 km 109 x larger than Earth weight 2 x 10
More information2. Basic assumptions for stellar atmospheres
. Basic assumptions for stellar atmospheres 1. geometry, stationarity. conservation of momentum, mass 3. conservation of energy 4. Local Thermodynamic Equilibrium 1 1. Geometry Stars as gaseous spheres
More informationObserver-Sun Angles. ), Solar altitude angle (α s. ) and solar azimuth angle (γ s )). θ z. = 90 o α s
Observer-Sun Angles Direction of Beam Radiation: The geometric relationships between a plane of any particular orientation relative to the earth at any time and the incoming beam solar radiation can be
More informationNeeds work : define boundary conditions and fluxes before, change slides Useful definitions and conservation equations
Needs work : define boundary conditions and fluxes before, change slides 1-2-3 Useful definitions and conservation equations Turbulent Kinetic energy The fluxes are crucial to define our boundary conditions,
More informationρ x + fv f 'w + F x ρ y fu + F y Fundamental Equation in z coordinate p = ρrt or pα = RT Du uv tanφ Dv Dt + u2 tanφ + vw a a = 1 p Dw Dt u2 + v 2
Fundamental Equation in z coordinate p = ρrt or pα = RT Du uv tanφ + uw Dt a a = 1 p ρ x + fv f 'w + F x Dv Dt + u2 tanφ + vw a a = 1 p ρ y fu + F y Dw Dt u2 + v 2 = 1 p a ρ z g + f 'u + F z Dρ Dt + ρ
More information(1) Over the course of a day, the sun angle at any particular place varies. Why?
(1) Over the course of a day, the sun angle at any particular place varies. Why? (Note: Although all responses below are true statements, only one of them actually explains the observation!) (A)The sun
More informationResponse to Unified Theory of Climate
Response to Unified Theory of Climate Dr. Daniel M. Sweger National College Introduction During the last two years that I have been teaching Environmental Science and attempting to explain global warming
More informationPractice Problems for Exam 3 (Solutions) 1. Let F(x, y) = xyi+(y 3x)j, and let C be the curve r(t) = ti+(3t t 2 )j for 0 t 2. Compute F dr.
1. Let F(x, y) xyi+(y 3x)j, and let be the curve r(t) ti+(3t t 2 )j for t 2. ompute F dr. Solution. F dr b a 2 2 F(r(t)) r (t) dt t(3t t 2 ), 3t t 2 3t 1, 3 2t dt t 3 dt 1 2 4 t4 4. 2. Evaluate the line
More informationE d. h, c o, k are all parameters from quantum physics. We need not worry about their precise definition here.
The actual form of Plank s law is: b db d b 5 e C C2 1 T 1 where: C 1 = 2hc o 2 = 3.7210 8 Wm /m 2 C 2 = hc o /k = 1.3910 mk Where: h, c o, k are all parameters from quantum physics. We need not worry
More information+ ω = 0, (1) (b) In geometric height coordinates in the rotating frame of the Earth, momentum balance for an inviscid fluid is given by
Problem Sheet 1: Due Thurs 3rd Feb 1. Primitive equations in different coordinate systems (a) Using Lagrangian considerations and starting from an infinitesimal mass element in cartesian coordinates (x,y,z)
More informationModels of ocean circulation are all based on the equations of motion.
Equations of motion Models of ocean circulation are all based on the equations of motion. Only in simple cases the equations of motion can be solved analytically, usually they must be solved numerically.
More informationCLIMATE AND CLIMATE CHANGE MIDTERM EXAM ATM S 211 FEB 9TH 2012 V1
CLIMATE AND CLIMATE CHANGE MIDTERM EXAM ATM S 211 FEB 9TH 2012 V1 Name: Student ID: Please answer the following questions on your Scantron Multiple Choice [1 point each] (1) The gases that contribute to
More information