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IES Exam 1 Lecture 2

EMR, Earth-Sun Fundamentals

TermDefinition
EMR Radiation Frequency is inversely proportional to wavelength
Shortwave Examples Gamma rays, cosmic rays, x-ray, UV
Longwave Examples Infrared spectrum, microwave spectrum, radio spectrum
Wein's Law Hotter the object, the shorter the wavelength
Stefan-Boltzmann's Law Hot objects emit more energy than cold objects
Sun v. Earth EMR Sun emits at a shorter wavelength and emits more than Earth
Earth's Energy Input Solar Radiation to Earth Shorter wavelengths UV, visible, shortwave infrared
Earth's Energy Output Earth's infrared emission to space
Solar Constant 1372 W/m^2
Outgoing EMR Amount 240 W/m^2
Surface Area Outgoing v. Incoming Surface area for outgoing is larger
Insolation Distribution by Latitude Low Latitudes (Equator) get more direct sunlight
Solar Distance v. Angle Distance doesn't matter, just angle
Low Latitude Net Radiation Gaining Energy
High Latitude Net Radiation Losing energy
Created by: Eliana.s
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