Equilibrium Temperature Of The Earth
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This powerpoint shows a simple calculation for the equilibrium temperature of the Earth assuming there are no greenhouse gases present.
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Black body radiation is electromagnetic radiation emitted from objects due to their internal heat. Max Planck introduced the concept that the energy of atomic oscillators that emit radiation inside a black body is quantized, meaning it can only take on discrete values. This resolved the ultraviolet catastrophe, where classical theories predicted infinite radiation at short wavelengths. Planck derived a theoretical expression for blackbody radiation intensity that matched experiments. It introduced the fundamental constant h, relating the energy of light to its frequency. This established the quantum nature of light and energy and was a breakthrough in physics.
Chapter 1 blackbody radiation
This document discusses key concepts relating to blackbody radiation. It begins by introducing the concept of a blackbody as an ideal absorber of electromagnetic radiation. It then describes Stefan's Law, which states that the total energy radiated by a blackbody is directly proportional to the fourth power of its thermodynamic temperature. Next, it explains Wein's Displacement Law, which establishes that the peak wavelength of blackbody radiation is inversely proportional to the temperature of the blackbody. The document provides formulas for both laws and gives examples of how they can be applied.
Chapter 1 blackbody radiation
This document discusses key concepts relating to blackbody radiation. It begins by introducing the concept of a blackbody as an ideal absorber of electromagnetic radiation. It then describes Stefan's Law, which states that the total energy radiated by a blackbody is directly proportional to the fourth power of its thermodynamic temperature. Next, it explains Wein's Displacement Law, which establishes that the peak wavelength of blackbody radiation is inversely proportional to the temperature of the blackbody. The document provides formulas for both laws and gives examples of how they can be applied.
Radiation heat transfer and clothing comfort
Radiation is a mode of heat transfer that does not require a medium. Thermal radiation is emitted from all objects based on their temperature and is characterized by properties like emissivity. Radiation plays a key role in heating the Earth's surface from the Sun. The amount of radiation emitted by an object increases with its temperature, as described by Stefan-Boltzmann law. Radiation interacts with textiles through absorption, emission, transmission, and scattering depending on fiber properties. Research aims to model radiation transfer through textiles and its role in thermal insulation and heat stress protection.
Stefan's Law
This document discusses verifying Stefan's law through an electrical experiment. Stefan's law states that the total heat radiated from a surface is proportional to the fourth power of the absolute temperature. The experiment involves measuring the radiant heat power (P) and resistance (R) of a tungsten filament. Taking the log of both sides of Stefan's law and the resistance equation allows creating a graph of logP vs logR. According to the law, the slope of this graph should be 4. The experiment finds the slope to be 3.90, close enough to 4 to verify Stefan's law.
013 fundamental of thermal radiation
This document provides an overview of fundamental radiation concepts. It defines thermal radiation and blackbody radiation, describing the idealized blackbody and Stefan-Boltzmann law. It also covers radiation intensity, radiative properties including emissivity and absorptivity, and Kirchhoff's law relating emissivity and absorptivity. The objectives are to classify electromagnetic radiation, understand blackbody radiation characteristics, and apply concepts of radiation intensity and surface radiative properties.
Radiation
- Radiation is the transfer of heat through electromagnetic waves between objects, even in a vacuum. Unlike conduction and convection, radiation can occur over distances without a medium.
- The rate of radiation heat transfer depends on the temperature of the objects - hotter objects radiate more energy than colder objects. All objects with temperatures above absolute zero radiate energy.
- Plank's law describes the spectral distribution of radiation emitted by a blackbody, which is the perfect emitter and absorber. It shows that radiation intensity peaks at shorter wavelengths as temperature increases.
Global warming
The document discusses the greenhouse effect and global warming. It presents the results of three polls:
1) 100% of respondents believe the planet is warming
2) 100% of respondents believe human activity has contributed to the warming
3) 80% of respondents believe there is significant controversy in the scientific community around climate change
It then provides a simple explanation of the greenhouse effect and how greenhouse gases like carbon dioxide trap infrared radiation and warm the planet. A two-layer model of the atmosphere and surface demonstrates how the atmosphere increases the planet's temperature above what it would be without an atmosphere.
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Equilibrium Temperature Of The Earth
- 1. Equilibrium Temperature of the Earth
- 3. Spectrum Graph of intensity versus wavelength or frequency Intensity Energy per unit area per unit time Unit of intensity is
- 5. Spectrum of sunlight striking the atmosphere and surface of the Earth
- 6. The fraction of light reflected from the surface of the Earth is called the albedo of the Earth
- 8. The sunlight strikes the earth on just one side as shown. Thus the total power being absorbed, Pabs, on the earth is Iabs times the area of a circle whose radius is the radius of the earth, Pabs = Iabs( R 2 ), where R is the radius of the earth.
- 9. The amount of power being radiated away, P rad , is P rad = I rad (4 R 2 ), where I rad is the intensity being emitted in units of kW/m 2 . Since there is thermal equilibrium, P abs = P rad or I abs ( R 2 ) = I rad (4 R 2 ).
- 10. Dividing through by R 2 yields I rad = I abs /4. The Stefan-Boltzmann law for a blackbody says I rad = T 4 , where T is the temperature of the blackbody and is the Stefan-Boltzmann constant ( = 5.67x10 -8 W/m 2. K 4 ).
- 11. Substituting yields T 4 = I abs /4 = 959 W/m 2 /4 = 240 W/m 2 Or T = 255 K = -18 o C