GY 101 wk3
GY 101 wk3 GY 101
Popular in Atmospheric Processes & Patterns
verified elite notetaker
Popular in Geography
One Day of Notes
verified elite notetaker
This 3 page Class Notes was uploaded by Elle Notetaker on Thursday February 4, 2016. The Class Notes belongs to GY 101 at University of Alabama - Tuscaloosa taught by Eben Broadbent in Fall 2016. Since its upload, it has received 151 views. For similar materials see Atmospheric Processes & Patterns in Geography at University of Alabama - Tuscaloosa.
Reviews for GY 101 wk3
Report this Material
What is Karma?
Karma is the currency of StudySoup.
You can buy or earn more Karma at anytime and redeem it for class notes, study guides, flashcards, and more!
Date Created: 02/04/16
GY101 notes from 2/3/2016 The sun is mostly Hydrogen (No way! that was sarcasm, for those of you who couldn’t tell.) Photosphere 9,900 Deg. F, surface of the sun. Energy the ability to do work. every activity requires energy typing, reading, breathing, etc. electromagnetic radiation of the energy the sun gives out, 1/ 2bill. of it is given to Earth as such. 8 min for light to get to us. Earth’s surface and atmos each take up some of the sun’s emr. TYpes of Energy a) kinetic throw an object, it has kinetic. moving energy. ex: light, heat, motion, electricity. b) potential ex. holding an object in the air, it’s got potential energy. PE comes from where an object is/ location. stored energy. ex: food, gas, firewood, battery, high pressure, reservoirs. power the amount of energy being used work moving something a distance by using force Rollercoaster: at top before you start going, you’ve got lots of potential energy. at the bottom of the hill, where you’re going fastest, you have a lot of kinetic energy. energy transfer mechanisms: how to move energy from pt a to pt. b. 3 main processes conduction, convection, radiation 1) conduction heat goes through substance w/out the molecules moving in direction of transfer. molecule to molecule shift of heat. heat going from a mug to your hand. goes to the ground, works best in solids (the molecules are touching & can pass off the energy easier. like making a bucket brigade when a house is on fire. The water moves, the people don’t. 2) convection heat moves when a liquid is mixed both liquids & gases. heat goes through a pot of boiling water, heating of the earth’s surface. fans are an example of this they move the air around to cool you off (unless they’re going slowly, in which case they make you hotter either way, they move energy and change temperatures in the area being affected.) molecules are moving around. 3) radiation moving energy without using physical mediums. the sun sends its energy to us through the black void of space via radiation. radiation is emitted by everything,, always. you feel the heat of a campfire even though you aren’t touching it that’s radiation. there are no molecules involved in this. at all. Radiation Characteristics: R. quantity the amount of energy being transferred. related to amplitude/wave height R quality wavelength distance between wave crests. ex: each color has its own wavelength of emr. electric and magnetic waves push each other along at the speed of light. electromagnetic spectrum range of radiation wavelengths, each type of wave with its own range. ex, visible light has a limited range of wavelengths, and microwaves have their own. Wavelengths range in length from the height of an atomic nucleus to that of Mt. Everest. It’s the really small ones that we tend to be worried about gamma radiation, xrays, ultraviolet. ORDER OF Lengths (short to long): gamma, Xrays, Ultraviolet, Visible light, infrared, microwaves, fm radio, then am radio waves, long radio waves the sun sends out all types of radiation at all times. yay! SteffanBoltzmann law an object’s radiation intensity is proportional to it’s temperature to the 4th power. units: watts/m². Blackbodies emit radiation perfectly (they’re only hypothetical right now, though). The amount and wavelengths of energies are defined by physical laws, and the radiation amount/intensity is related to the temperature of the object. The temperatureradiation proportion is NOT linear, and is regulated by the SteffanBoltzmann law. Earth and the Sun are similar to blackbodies because they emit radiation that almost matches the SB law. blackbodies are theoretical things whose radiation matches the steffanboltzmann law perfectly. Graybodies they send out some percentage of what blackbodies would emit. liquids & solids are typically graybodies. Electromagnetic Radiation (EMR) a combination of magnetic & electric waves, moving together but on separate planes, propel each other forward at the speed of light. EMR travels as a wave/series of waves, with all the required properties. (You know amplitude, wavelength, frequency all that jazz.) Emissivity the percent of energy a substance sends out, as related to what it would send out if said object were a blackbody. most stuff will have a .9 emissivity or above. radiation intensity is a function of temperature and emissivity. EMR doesn’t slow down or anything as it gets closer to the Earth it spreads out. (A flashlight’s illumination is stronger as you get closer to it, but it will cover a lot more area if you move the light back some. In the same way, radiation is inversely proportional to the distance between the objects of interest squared. In other words, radiation is proportional to 1/d² this is called the inverse square law. Solar constant a measure of flux density and the amount of Solar EMR the Earth system gets. It comes in constantly, at a rate of roughly 1,366 watts/m² on the big circle of the Earth system. It’s kind of confusing, so here’s a picture for you.
Are you sure you want to buy this material for
You're already Subscribed!
Looks like you've already subscribed to StudySoup, you won't need to purchase another subscription to get this material. To access this material simply click 'View Full Document'