Chapter 2: The global ledger of radiation and heat

PROPERTIES OF RADIATION Everything radiates at all wavelengths! This includes the Sun, Earth, a candy bar, even us Fortunately, most objects don t radiate a lot of X-rays, gamma rays, etc... However, different objects: Emit different amounts of radiation, and. Emit their maximum radiation at different wavelengths (don t confuse these two differences) So what s the determining factor? TEMPERATURE!

PROPERTIES OF RADIATION 2 EASY RULES: 1. The higher the temperature, the more radiation an object will emit (Stephan-Boltzman Law) 2. Higher temperature result in radiation being concentrated at shorter wavelength (Wien s Law)

Radiation Energy Transfer by Electromagnetic Waves Electromagnetic Spectrum UV VIOLET RED IR WAVELENGTH FREQUENCY ENERGY

PROPERTIES OF RADIATION Sun: 10,000 F (solar, shortwave radiation) 1. lots of radiation; 2. peak radiation in visible range Earth: 60 F (terrestrial, longwave radiation) 1. some (but much less) radiation; 2. peak radiation in infrared range

LOWER HIGHER

Transparency of the atmosphere by wavelength and atmospheric windows

SOLAR RADIATION & GEOMETRY Not all parts of Earth receive the same amounts of radiation. Why? TILT of our planet, 23.5

SOLAR RADIATION AND TILT

EARTH S SEASONS

LAND OF THE MIDNIGHT SUN

Mechanisms of Energy Transfer (Heating): Conduction: Transfer of kinetic or vibrational energy by direct molecular collisions. What could maximize conduction efficiency? Convection: Spontaneous transfer of thermal energy by turbulent mixing in fluids. What conditions might maximize convection? Radiation: Transfer of energy by electromagnetic waves. Only mechanism that doesn t need a medium for transfer. What could prevent radiative transfer? (Heat describes energy flow from hot -> cold, not amount of energy and object has)

How does direct radiation from the sun warm a cup of water (PS 2)??

Simple Thermodynamic Relationships P( in W) = Power = Energy / time Q(in J)=Total Energy= Power x time x area P A W 2 m incoming solar radiation density (power/are a) Q Q P A mc t T A 1 T P t A m c A 1

Assumptions in calculating Temp. warming: No significant net heat lost by conduction, convection, or radiation (this is BS except for rare special circumstances) All incident solar radiation is absorbed Uniform temperature of object Perfect styrofoam insulator Typical Heat Capacities: J/kg/ o C cal/g/ o C Substance or J/kg/K or cal/g/k Water (0 o C to 100 o C) 4186 1.000 Methyl Alcohol 2549 0.609 Ice (-10 o C to 0 o C) 2093 0.500 Steam (100 o C) 2009 0.480 Benzene 1750 0.418 Wood (typical) 1674 0.400 Soil (typical) 1046 0.250 Air (50 o C) 1046 0.250 Aluminum 900 0.215 Marble 858 0.205 Glass (typical) 837 0.200 Iron/Steel 452 0.108 Copper 387 0.0924 Silver 236 0.0564 Mercury 138 0.0330 Gold 130 0.0310 Lead 128 0.0305

EARTH S ENERGY BUDGET Energy from the Sun reaches the top of Earth s atmosphere Does all of it reach the surface? NO For example Ozone (O 3 ) absorbs UV Clouds and gases scatter, absorb, reflect other types of radiation Still, a lot of radiation (energy) reaches the surface of our planet.

NORTH POLE EQUATOR SOUTH POLE Most of the incoming solar radiation is absorbed at the Tropics

TERRESTRIAL RADIATION Amount of terrestrial radiation emitted from Earth s surface and atmosphere is dependent on temperature More terrestrial radiation emitted near equator (warmer) Less terrestrial radiation emitted near poles (colder)

NORTH POLE EQUATOR SOUTH POLE

Earth s Annual Energy Budget

EARTH S ENERGY BUDGET Because of the differences in incoming/outgoing radiation on the Earth, we have an energy imbalance between the polar regions and the Tropics. So winds and ocean currents exist to transport heat from the equator to the poles. TO CREATE AN ENERGY BALANCE

NORTH POLE EQUATOR SOUTH POLE

Average Emitted infrared radiation

Incoming solar radiation for August

Solar radiation absorbed yesterday

August solar radiation absorbed by surface

Sea Surface Temperatures

Sea Surface Temperature Anomaly