1 NATS 101 Lecture 5 Radiation

2 Review Items Heat Transfer Latent Heat

3 Modes of Heat Transfer Energy is only converted from one form to another or transferred from one place to another. Energy is transferred from hot to cold. Conduction - Molecules colliding; most efficient at interface. Convection - Requires movement of a fluid or gas.

4 Latent Heat Energy associated with phase of matter. Must be either added to or taken from a substance when it changes its phase. –To turn liquid water into solid ice, must remove energy from the liquid water. –To turn liquid water into vapor, must add a lot of energy to the liquid water.

5 Radiation Any object that has a temperature greater than 0 K, emits radiation. This radiation is in the form of electromagnetic waves, produced by the acceleration of electric charges. These waves don’t need matter in order to propagate; they move at the “speed of light” (3x10 5 km/sec) in a vacuum.

6 Electromagnetic Waves Two important aspects of waves are: –What kind: Wavelength or distance between peaks. –How much: Amplitude or distance between peaks and valleys. Wavelength AmplitudeFrequency

7 Why Electromagnetic Waves? Radiation has an Electric Field Component and a Magnetic Field Component –Electric Field is Perpendicular to Magnetic Field

8 Photons NOT TO CONFUSE YOU, but… Can also think of radiation as individual packets of energy or PHOTONS. In simplistic terms, radiation with shorter wavelengths corresponds to photons with more energy (or more BB’s per second) and with higher wave amplitude to bigger BB’s

9 Electromagnetic Spectrum WAVELENGTH Danielson, Fig Wavelengths of Meteorological Significance

10 Radiation Effects on Humans Danielson, Fig

11 Emitted Spectrum White Light from Flash Light PurpleGreen Red Emitted radiation has many wavelengths. Prism (Danielson, Fig. 3.14)

12 Plank’s Law: Emitted Spectrum Energy from Sun is spread unevenly over all wavelengths. Wavelength Energy Emitted Emission spectrum of Sun Ahrens, Fig. 2.7 Planck’s Law

13 Planck’s Law and Wien’s Law The hotter the object, the shorter the brightest wavelength. Danielson, Fig. 3.19

14 Wien’s Law Relates the wavelength of maximum emission to the temperature of mass MAX = (0.29  10 4  m K)  T -1 Warmer Objects => Shorter Wavelengths Sun-visible light MAX = (0.29  10 4  m K)  (5800 K) -1  0.5  m Earth-infrared radiation MAX = (0.29  10 4  m K)  (290 K) -1  10  m

15 Wien’s Law What is the radiative temperature of an incandescent bulb whose wavelength of maximum emission is near 1.0  m ? Apply Wien’s Law: MAX = (0.29  10 4  m K)  T -1 Temperature of glowing tungsten filament T= (0.29  10 4  m K)  ( MAX ) -1 T= (0.29  10 4  m K)  (1.0  m) -1  2900K

16 Stefan-Boltzmann’s (SB) Law The hotter the object, the more radiation emitted. Double the temperature  Total emitted radiation increases by a factor of 16! Stefan-Boltzmann’s Law E= (5.67  Wm -2 K -4 )  T 4 E=2  2  2  2=16 4 times Sun Temp: 6000K Earth Temp: 300K Aguado, Fig. 2-7

17 How Much More Energy is Emitted by the Sun per m 2 Than the Earth? Apply Stefan-Boltzman Law The Sun is 160,000 Times More Energetic per m 2 than the Earth, Plus Its Area is Mucho Bigger!

18 Radiative Equilibrium Radiation absorbed by an object increases the energy of the object. –Increased energy causes temperature to increase (warming). Radiation emitted by an object decreases the energy of the object. –Decreased energy causes temperature to decrease (cooling).

19 Radiative Equilibrium (cont.) When the energy absorbed equals energy emitted, this is called Radiative Equilibrium. The corresponding temperature is the Radiative Equilibrium Temperature. Concept is analogous to a bathtub with the faucet running and the drain unplugged. If water in exceeds water out, level rises. If water in is less than water out, level falls. If water in equals water out, level is constant or at an equilibrium level.

20 Modes of Heat Transfer Williams, p. 19 Latent Heat

21 Key Points Radiation is emitted from all objects that have temperatures warmer than absolute zero (0 K). Wien’s Law: wavelength of maximum emission MAX = (0.29  10 4  m K)  T -1 Stefan-Boltzmann Law: total energy emission E= (5.67  W/m 2 )  T 4

22 Key Points Radiative equilibrium and temperature Energy In = Energy Out (Eq. Temp.) Three modes of heat transfer Conduction: molecule-to-molecule Convection: fluid motion Radiation: electromagnetic waves Heat transfer works to equilibrate temperature differences

23 Reading Assignment Ahrens Pages Problems 2.10, 2.11, 2.12