ELECTROMAGNETIC SPECTRUM - Earth 002 Tuesday January 26th...

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Earth 002 Tuesday, January 26th, 1999 Announcements: Lecture notes: HEAT ENGINES Interior --> radioactive decay Solar Energy --> generated by the sun Distance from the sun is very important--farther from the sun, the colder it'll be Albedo -reflectivity of the planet ELECTROMAGNETIC SPECTRUM In the electromagnetic spectrum, light appears to travel as a wave Light is divided into many different wavelengths High Frequency --> Short Wavelengths (ex. gamma rays, x-rays) Low Frequency --> Long Wavelengths (ex. microwaves, radio waves) Visible lights wavelengths are between 400-700 nanometers (.4-.7 meters) long
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Short Wavelengths-->Higher Frequency-->More Energy Long Wavelengths-->Lower Frequency-->Less Energy ENERGY What governs how much energy we get? Blackbody -a perfect emitter and/or perfect absorber Hot bodies emit a higher temperature
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Unformatted text preview: • Short wavelengths-->Higher frequency-->More Energy-->Higher Temperature • Total energy flux of any blackbody: Ftot = 6T^4 (T=temp, 6= 5.67 * 10^-8) • SUN Ftot = 6.0 * 10^7 w/m2 (watts per meter squared) • EARTH Ftot = 1370 w/m2 (watts per meter squared) INVERSE SQUARE LAW • So (Ro/R)^2 = S (So=sun's energy flux, Ro=sun's radius, S=total energy emitted by sun) • The farther from the sun, the less energy received • Triple the distance from the sun --> 1/9 the original energy • Double the distance from the sun --> 1/4 the original energy ENERGY BALANCE OFF EARTH • Ein = Eout • S/4 (1-A) = ? 6(Te^4) (S=1370, A=.3, 6=5.67*10^-8, Te=-18 C) • shorter wavelength->higher frequency->more energy->higher temperature • HOT BODY RADIATES MORE ENERGY AT SHORTER WAVELENGTHS...
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