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GRG 366C Exam Review

by: Cassidy Schap

GRG 366C Exam Review GRG 366C

Cassidy Schap
GPA 3.78
Comparative Ecosystems
Thoralf Meyer

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About this Document

This is a review for the Comparative Ecosystems exam covering the basics of ecology.
Comparative Ecosystems
Thoralf Meyer
Study Guide
50 ?




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This 2 page Study Guide was uploaded by Cassidy Schap on Sunday September 27, 2015. The Study Guide belongs to GRG 366C at University of Texas at Austin taught by Thoralf Meyer in Summer 2015. Since its upload, it has received 47 views. For similar materials see Comparative Ecosystems in Geography at University of Texas at Austin.


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Date Created: 09/27/15
Basics of Ecology Test review De ne Ecology The study of interactions among organisms and between their abiotic environment First Law of Thermodynamics Energy cannot be created nor destroyed only changed in form CAM A type of photosynthesis Crassulacean acid metabolism Biome Areas with similar climatic conditions de ned by geographic location location determines radiation budget solar terrestrial and availability of water Biomes determined by latitude altitude temperature availability of water Biome Landscape Ecosystem Community Population Individual Two major plant nutrients Nitrogen phosphorous Ecosystem disturbances natural Flooding seismic events landslides avalanches re grazingbrowsing extreme climatic events others Albedo Measure of re ectivity Trophic level Indicates the general availability of nutrients to an ecosystem oligotroph mesotroph eutroph The sum within a given ecosystem is always constant De ning Ecosystem The size of a system depends on what one wants to study It39s a question of spatial 3 dimensional temporal scale Solar radiation Thermal radiation Net radiation of the planet Net radiation the amount in full that is available for most every ecological process Net Plant Photosynthesis Heat Storage Sensible Heat Latent Heat of vaporization Net Plant Photosynthesis Soil Respiration Carbon Storage Carbon Budget Latent Het Runo Drainage Water Storage Water Balance Radiation The electromagnetic energy from the Sun travels in eight minutes across the intervening 93 million miles 150 million km of space to the Earth The Sun produces a continuous spectrum of electromagnetic radiation ranging from very short extremely high frequency gamma and cosmic waves to long very low frequency radio waves Frequency x Wavelength Speed of Light Wavelength measured in nm Visible light from 380 nm 720 nm Gamma Xray Ultraviolet Visible Spectrum VioletBlueGreenYellowRed Infrared Characterize the energy of the Sun Think of Sun as a 6000 K quotblackbodyquot a theoretical construct which radiates energy at the maximum possible rate per unit area at each wavelength for any given temperature The total emitted radiation M from a blackbody is proportional to the fourth power of its absolute temperature The is known as the Stefan Boltzmann law and is expressed as MoTquot4 Where 0 is the StefanBoltzmann constant 56697 x 10quot8 W mquot2 Kquot4 Thus the amount of energy emitted by an object such as the Sun or the Earth is a function of its temperature Thermonuclear fusion taking place on the surface of the Sun yields a continuous spectrum of electromagnetic energy The 57706000 kelvin K temperature of this process produces a large amount of relatively short wavelength energy travels through the vacuum of space at the speed of light Some of this energy is intercepted by the Earth where it interacts with the atmosphere and surface materials The Earth re ects some of the energy directly back out to space or it may absorb the short wavelength energy


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