Which picture shows the larger flux of blue circles?

Similar documents
Global Energy Balance. GEOG/ENST 2331: Lecture 4 Ahrens: Chapter 2

Energy and Radiation. GEOG/ENST 2331 Lecture 3 Ahrens: Chapter 2

Earth: the Goldilocks Planet

Blackbody Radiation. A substance that absorbs all incident wavelengths completely is called a blackbody.

Friday 8 September, :00-4:00 Class#05

MASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Physics Problem Solving 10: The Greenhouse Effect. Section Table and Group

Lecture 2 Global and Zonal-mean Energy Balance

Atmospheric "greenhouse effect" - How the presence of an atmosphere makes Earth's surface warmer

Monday 9 September, :30-11:30 Class#03

Take away concepts. What is Energy? Solar Radiation Emission and Absorption. Energy: The ability to do work

Radiative Equilibrium Models. Solar radiation reflected by the earth back to space. Solar radiation absorbed by the earth

Atmospheric "greenhouse effect" - How the presence of an atmosphere makes Earth's surface warmer

Radiation Conduction Convection

1. Weather and climate.

2. Energy Balance. 1. All substances radiate unless their temperature is at absolute zero (0 K). Gases radiate at specific frequencies, while solids

Mon April 17 Announcements: bring calculator to class from now on (in-class activities, tests) HW#2 due Thursday

Lecture 3: Global Energy Cycle

Understanding the Greenhouse Effect

2. Illustration of Atmospheric Greenhouse Effect with Simple Models

Lecture 5: Greenhouse Effect

Earth Systems Science Chapter 3

Lecture 4: Global Energy Balance

Lecture 5: Greenhouse Effect

Lecture 4: Global Energy Balance. Global Energy Balance. Solar Flux and Flux Density. Blackbody Radiation Layer Model.

Mon Oct 20. Today: radiation and temperature (cont) sun-earth geometry energy balance >> conceptual model of climate change Tues:

Astro 210 Lecture 16 October 1, 2010

Lecture 3a: Surface Energy Balance

di λ ds = ρk λi λ B λ (T ) + ρk λ dz' )= B λ (T(z'))e I λ (z TOA + k λ Longwave radiative transfer Longwave radiative transfer

Lecture 3a: Surface Energy Balance

Agronomy 406 World Climates January 11, 2018

ESE / GE 148a: Introduction to Climate. Organizational Details - I

Lecture 4: Radiation Transfer

ATMOS 5140 Lecture 7 Chapter 6

Astro 210 Lecture 16 Feb 23, 2018

Lecture 6. Solar vs. terrestrial radiation and the bare rock climate model.

Electromagnetic Radiation. Radiation and the Planetary Energy Balance. Electromagnetic Spectrum of the Sun

Radiative Balance and the Faint Young Sun Paradox

Remote Sensing C. Rank: Points: Science Olympiad North Regional Tournament at the University of Florida. Name(s): Team Name: School Name:

Temperature Scales

Radiation in climate models.

Learning goals. Good absorbers are good emitters Albedo, and energy absorbed, changes equilibrium temperature

Energy, Temperature, & Heat. Energy, Temperature, & Heat. Temperature Scales 1/17/11

THE EXOSPHERIC HEAT BUDGET

Outline. Stock Flow and temperature. Earth as a black body. Equation models for earth s temperature. Balancing earth s energy flows.

TOPIC # 6 The RADIATION LAWS

Earth s Energy Balance and the Atmosphere

INTRODUCTION Radiation differs from conduction and convection in that it does not require the presence of a material medium to take place.

Radiation in the atmosphere

aka Light Properties of Light are simultaneously

IB Physics Lesson Year Two: Standards from IB Subject Guide beginning 2016

Teaching Energy Balance using Round Numbers: A Quantitative Approach to the Greenhouse Effect and Global Warming

MNFFY 221/SIF 4082 Energy and Environmental Physics. 2002

Lecture Outline. Energy 9/25/12

Oppgavesett kap. 4 (1 av 2) GEF2200

PTYS 214 Spring Announcements. Midterm 3 next Thursday! Midterms 4 and 5 more spread out

GE510 Physical Principles of the Envt

Chapter 3 Energy Balance and Temperature. Astro 9601

MATH 392, Seminar in Mathematics and Climate Computer Project #1: Energy Balance Models

PTYS 214 Fall Announcements

Lecture 2: Global Energy Cycle

Name... Class... Date...

Radiative heat transfer

With certain caveats (described later) an object absorbs as effectively as it emits

The current climate epoch: The Holocene

Modeling of Environmental Systems

Chapter 3 Energy Balance and Temperature. Topics to be covered

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.

Lecture # 04 January 27, 2010, Wednesday Energy & Radiation

COMPUTER METHODS AND MODELING IN GEOLOGY MODELING EARTH'S TEMPERATURE

CLIMATE AND CLIMATE CHANGE MIDTERM EXAM ATM S 211 FEB 9TH 2012 V1

Thursday, November 1st.

1) The energy balance at the TOA is: 4 (1 α) = σt (1 0.3) = ( ) 4. (1 α) 4σ = ( S 0 = 255 T 1

Sources of radiation

Let s make a simple climate model for Earth.

TSOKOS READING ACTIVITY Section 7-2: The Greenhouse Effect and Global Warming (8 points)

P607 Climate and Energy (Dr. H. Coe)

8.5 GREENHOUSE EFFECT 8.6 GLOBAL WARMING HW/Study Packet

TOPIC # 7 The RADIATION LAWS

Earth s Energy Budget: How Is the Temperature of Earth Controlled?

Name(s) Period Date. Earth s Energy Budget: How Is the Temperature of Earth Controlled?

ATMO/OPTI 656b Spring 2009

Today. Spectra. Thermal Radiation. Wien s Law. Stefan-Boltzmann Law. Kirchoff s Laws. Emission and Absorption. Spectra & Composition

Thermal Radiation By: Prof. K M Joshi

Hand in Question sheets with answer booklets Calculators allowed Mobile telephones or other devices not allowed

ME 476 Solar Energy UNIT TWO THERMAL RADIATION

In the News:

ESS15 Lecture 7. The Greenhouse effect.

Lecture 3: Emission and absorption

- matter-energy interactions. - global radiation balance. Further Reading: Chapter 04 of the text book. Outline. - shortwave radiation balance

MATH 303, Mathematical Models Computer Project #3: Energy Balance Models

A Warm Up Exercise. A Warm Up Exercise. A Warm Up Exercise. A Warm Up Exercise. The Solar Flux

Spectrum of Radiation. Importance of Radiation Transfer. Radiation Intensity and Wavelength. Lecture 3: Atmospheric Radiative Transfer and Climate

Wednesday, September 8, 2010 Infrared Trapping the Greenhouse Effect

Lecture 3: Atmospheric Radiative Transfer and Climate

Lecture 9: Climate Sensitivity and Feedback Mechanisms

WRAP UP OF TOPIC #5... ELECTROMANGETIC RADAITAION & THE ELECTROMAGNETIC SPECTRUM

4. Zero-dimensional Model of Earth s Temperature

M.Sc. in Meteorology. Physical Meteorology Prof Peter Lynch. Mathematical Computation Laboratory Dept. of Maths. Physics, UCD, Belfield.

The greenhouse effect

Earth: A Dynamic Planet A. Solar and terrestrial radiation

Transcription:

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 a Climate Model The energy of a gas is a function of its temperature only (vice versa). Thus, if the atmosphere s T changes, its energy balance has changed. If we can describe the sources and sinks of energy, we can predict T.

Radiation Absorption, Emission, Temperature - emission Characteristic of a body s T --is an energy loss mechanism - absorption Induces more atomic/molecular motion Increases a body s T --is an energy source

Interactions of Radiation and Matter 1. Absorption causes matter to warm 2. Emission causes matter to cool 3. Transmission no interaction 4. Scattering direction of propagation altered like reflection but more general All processes happen on Earth and are important in considering the energy balance of the planet.

Earth Energy Balance Model: Take 1 Simplifying assumptions 1. Radiation is sole form of energy transfer 2. Solar radiation is only energy input, constant 3. Everywhere on Earth receives same average energy 4. Atmosphere plays no role 5. Earth is in radiative equilibrium Energy flow in equals energy flow out

Emission Spectrum body Wavelength selector Photon counter Flux (photons/m 2 /s) wavelength

Blackbody Radiation: Wien s Law the peak wavelength... Radiation Flux (W/m 2 ) is inversely proportional to the object s temperature

Blackbody Radiation: Stefan-Boltzmann Radiation Flux (W/m 2 ) Area under curve is the total emission flux proportional to T 4

Energy Balance: Halfway Done Energy Flux In = Energy Flux Out F in = F out F in = σt 4 Earth Assume Earth radiates like a blackbody

The sun s emission spectrum maximizes at a λ of ~ 0.5 µm. The sun s temperature is 1. ~ 1500 K 2. ~ 6000 K 3. ~ 15,000 K 33% 33% 33% ~ 1500 K ~ 6000 K ~ 15,000 K

Announcements Should have received emails from me No class Thurs Jan 31 Attend Focus the Nation First exam scheduled for Fri Feb 8 Review session on Thurs Feb 7 in class Any Device ID starting with 0, will be recorded without the 0.

Energy Balance: Halfway Done Energy Flux In = Energy Flux Out F in = F out F in = σt 4 Earth Assume Earth radiates like a blackbody

Earth s Energy Balance: Towards F IN R S D SE Need to account for a) Earth-Sun distance (inverse square law), b) Earth intercepts fraction of total solar flux at D SE c) Earth reflects some of the intercepted radiation

Solar Emission Flux The sun emits about 6.3 X 10 7 W/m 2 of radiant energy How are we still here?

Radiant Energy Flux Far From Source r obj ** vs d 1 d 2 **this picture is a bit misleading Flux decreases as inverse square of distance from source F d! d " = F * 1 d # $ d 2 1 % 2 & 2

Spectrum of Solar Radiation Flux (measured at Earth) Flux Distribution Outside of atmosphere Reaching Earth s surface Perfect blackbody

Earth s Energy Balance: Towards F IN R S D SE Need to account for a) Earth-Sun distance (inverse square law), b) Earth intercepts fraction of total solar flux at D SE c) Earth reflects some of the intercepted radiation

Both the sphere and disc have the same radius, which will intercept more radiation? Area = πr 2 44% 39% Area = 2πr 2 17% 1. disc 2. sphere 3. both intercept same disc sphere both intercept same

Earth s Energy Balance: Earth Sun Geometry

Earth s Energy Balance No Atmosphere F in = F out S o ( 1" A) 4 4 =! T E T E = & $ % S o 1 ( 1' A) 4 4( #! " Same approach for ANY planet!

Earth s Energy Balance No Atmosphere T E = & $ % Plug in known values for S o, A, and σ and predict S o 1 ( 1' A) 4 4( T E ~ 256 K #! " (-17 o C below freezing) Not a very good prediction! What s wrong with our model?

Energy Balance Cartoon S o /4 = 341 Wm -2 (S o /4)A = 96 Wm -2 F IN ~ 245 Wm -2 Planet F out = σt E 4 Bare rock Model (i.e. no atmosphere) Predict T E ~ 256 K when atmosphere is neglected

Where did we go wrong? Examine the validity of our assumptions 1. Radiation only form of energy OK for global energy balance 2. Sun only energy source, constant Very good for average state 3. Solar energy deposited uniformly OK for global average energy balance 4. Atmosphere plays no role Hmmm 5. F in = F out Good for global long-term average

The Greenhouse Effect T true T bare rock 289 K 256 K = 33 K The atmosphere increases the average surface temperature by about 13% Can we explain the physics and predict the right T?

Announcements Graded Problem Set 1 handed back tomorrow in discussion Problem Set 2 now/soon available, DUE Friday Feb 1 in discussion SHOW WORK! Reading Chapter 3

Global Climate Model: Take 2 Let s model the Earth system as a planetary surface with an absorbing atmosphere above the surface. S o /4 (S o /4)A (1-ε) F sf OUT εf atm OUT Atmosphere T atm F sf IN F sf OUT εf atm OUT Surface T sf

Global Climate Model: Take 2 Simplifying Assumptions 1. The atmosphere absorbs only Outgoing Long wave Radiation (no absorption of solar radiation) 2. The atmosphere absorbs the same fraction of OLR at each wavelength. 3. The atmosphere has a uniform temperature. 4. F in = F out for each component and whole system.

Non-Blackbodies (<100% absorption) - emission - absorption The same springs (matter) forced with three different frequencies

Kirchoff s Law: Imperfect Blackbody A body will only emit the same wavelengths it absorbs. Radiation Flux Distribution True spectrum Ideal Blackbody spectrum

Global Climate Model: Take 2 A planetary surface with an absorbing atmosphere above the surface. (see pg 43 of textbook) S o /4 (S o /4)A (1-ε)F sf OUT εσt atm 4 S o (1-A)/4 Atmosphere T atm F sf OUT = σt sf 4 εσt atm 4 Surface T sf

Global Climate Model: Take 2 ( ) 4 1 2 1 4 1!!!! " # $ $ $ $ % & ' ( ) * +, - - =. / A S T o Wear it, sleep on it, put it on your cereal box,

Global Climate Model: Take 2 sf T Earth ~ & $ 247 $ $,. / * 1 - $ % + 2 ) ' ( #!!!! " 1 4 If ε ~ 0.75, then T Earth ~ 289 K

If the atmosphere s absorptivity, ε, increases, Earth s surface T 1. Increases 2. Decreases 3. Stays the same 59% 37% sf T Earth ~ & # $ 247! $! $,. ) / 1! $ * - ' % + 2 (! " 1 4 Increases Decreases 4% Stays the same

1-Layer Model Summary 1. An OLR absorbing atmosphere slows the net energy flow out from surface (relative to no atm). 2. An increase in atmosphere s absorptivity causes surface T to increase. 3. Radiation reaching space from the Earth is a combination of emission from a warm surface and colder atmosphere. It must be equivalent to 245 W/m 2 at equilibrium.