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## Environmental Geology: Energy Balances

by: Justin Notetaker

31

0

4

# Environmental Geology: Energy Balances GEOL 207

Marketplace > Ball State University > Geology > GEOL 207 > Environmental Geology Energy Balances
Justin Notetaker
BSU
GPA 3.0

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Discuss the basics for energy balances on earth, using simple equations.
COURSE
Environmental Geology - Geological/Geochemica
PROF.
Neumann
TYPE
Class Notes
PAGES
4
WORDS
CONCEPTS
Energy, balances, Input, output, Blackbody, temperature, Albedo, flux, Kelvin, sun, EARTH
KARMA
25 ?

## Popular in Geology

This 4 page Class Notes was uploaded by Justin Notetaker on Thursday January 28, 2016. The Class Notes belongs to GEOL 207 at Ball State University taught by Neumann in Winter 2016. Since its upload, it has received 31 views. For similar materials see Environmental Geology - Geological/Geochemica in Geology at Ball State University.

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Date Created: 01/28/16
GEOL 204 Environmental geology Energy Balances What goes in and what goes out? Input = Output Energy input (earth) = energy output (earth) Radiation: provides energy to the earth Electromagnetic waves Wavelength = Frequency = Speed = 3x10^8 m/s Wavelength * Frequency = speed Frequency = Speed / wavelength Photons (Duality) / (Light) Particle Pulse h = Plank Constant = 6.63*10^-34 j/s Energy (E) = h * frequency High Energy  Will cause chemical reaction Low Energy  Will cause more vibration Flux (F) or (S) – Energy per area per time Area: Watt/cm Time: /s Perpendicular to the surface to calculate Flex 1370 Watts/ m^2 = earth receives from the sun 6.3x10^7 Watts/m^2 = the sun How far away from the sun are we? The closer to the sun the more radiation. S = S(o) * [r(o) / r]^2 How warm is the sun and how warm is the earth? How do we measure it and how does it change? Blackbody Radiation (Red Dominant Visible) Wien’s Law Wavelength = 2898 / T T= temperature in kelvin Sun = 5780 Kelvin (K) Sun = 5780 / 2898 = 501 nanometers Earth = 288 K Earth = 288 / 2898 = 10,062 nm Visible Light = 400 – 700 nm Infrared > 700 nm 40% Ultraviolet > 10% Stefan – Boltzmann Equation F = Sigma *(T^4) Sigma = 6.7x10^-8 Watts/m^2/K^4  CONSTANT Energy that goes in and out depends on: - Flux (F) or (S) = CONSTANT - Albedo = 30% or 0.3 - Greenhouse Effect OUTGOING ENERGY / Flux F = Sigma * T(earth)^4 F = 4*(pi)*R^2 * Sigma*T(earth)^4 INCOMING ENERGY / Flux F = S*(pi)R^2

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