GRG 366C Lecture 1 Notes
GRG 366C Lecture 1 Notes GRG 366C
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This 2 page Class Notes was uploaded by Cassidy Schap on Sunday September 27, 2015. The Class Notes belongs to GRG 366C at University of Texas at Austin taught by Thoralf Meyer in Summer 2015. Since its upload, it has received 19 views. For similar materials see Comparative Ecosystems in Geography at University of Texas at Austin.
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Date Created: 09/27/15
Lecture 01 The Basics of Ecology De nition the study of the interactions among organisms and between organisms and their abiotic enviro 1st law of thermo energy can not be lost Changes from one form to another The sum of all energy is constant CAM plants crassuacean acid metabolism a type of photosynthesis Biome areas with similar climactic conditions De ned by geographic location Location determined radiation budget solar terrestrial and the availability of water Trophic level indicates the general level of availability of nutrients in an ecosystem oligotroph mesotroph eutroph The ow is from high concentration to low concentration and some is lost as it uctuates The sum of energy within a given ecosystem is always constant The size of the ecosystem is determined by what you re looking for Time scale is also determined by what you re trying to nd out Solar radiation thermal radiation net radiation Net plant photosynthesis quot one of the few processes that take non organic matter and convert it to organic matter some of the incoming solar radiation is stored as heat in the form of latent heat and sensible heat latent heat is the amount of energy that is needed to vaporize liquid water the carbon budget is made up of three things photosynthesis soil respiration carbon storage places carbon is stored terrestrial ecosystems atmosphere and oceans water balance latent heat runoff drainage water storage radiation sun emits continuous electromagnetic radiation Ranges from v short to extremely high frequency waves Gamma rays cosmic waves radio waves visible light etc speed of light frequency x wavelength it is possible to measure the energy of the sun think of the sun at a 6000 K Kelvin blackbody blackbody a theoretical construct which radiates energy at the maximum possible rate per unit area at each wavelength for any given temp the total emitted radiation from a blackbody is proportional to the fourth power of its absolute temp check PPT for the StefanBoltzmann law amount of energy emitted by an object like the sun or the earth is a function of it s temperature energy measurements in Kelvin thermonuclear fusion taking place on the surface of the sun gives constant energy the 57706000 K temp of this process produces a large amount of relatively short wavelength energy thst travels through space at the speed of light earth absorbs some of the radiation and re ects back the rest we can determine the max wavelength of an object based on Wein s displacement law check PPT for Wein s law blackbody radiation curves for several objects including the sun and the earth which approximate 6000K and 300K respectively the area under each curve is summed as the total radiation energy