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	Radiation Laws
		The primary law governing flbody radiation is the Planck Radiation Law, which governs the intensity of radiation emitted by unit surface area into a fixed direction (solid angle) from the flbody as a function of wavelength for a fixed temperature.
		The Wien Law gives the wavelength of the peak of the radiation distribution, while the Stefan-Boltzmann Law gives the total energy being emitted at all wavelengths by the flbody (which is the area under the Planck Law curve).
		Thus, the Wien Law explains the shift of the peak to shorter wavelengths as the temperature increases, while the Stefan-Boltzmann Law explains the growth in the height of the curve as the temperature increases.
	csep10.phys.utk.edu /astr162/lect/light/radiation.html (530 words)

	[No title]
		Curie's law (P. Curie) The susceptibility of a paramagnetic substance is inversely proportional to the thermodynamic temperature of the substance.
		law of reflection For a wavefront intersecting a reflecting surface, the angle of incidence is equal to the angle of reflection.
		Malus's law (E.L. Malus) The light intensity travelling through a polarizer is proportional to the initial intensity of the light and the square of the cosine of the angle between the polarization of the light ray and the polarization axis of the polarizer.
	users.rcn.com /zap.dnai/laws.txt (7313 words)

	CalendarHome.com - Joseph Stefan - Calendar Encyclopedia (Site not responding. Last check: )
		Stefan was born in an outskirt village St Peter (Slovene Sveti Peter) near Ebenthal (Slovene Žrelec) (today a district of Klagenfurt) (Celovec) in the Austrian Empire (now in Austria) to father Aleš (Aleksander) Stefan, born in 1805 and mother Marija Startinik, born 1815.
		In 1884 the law derived theoretically in the framework of thermodynamics by his student Ludwig Boltzmann and hence known as the Stefan-Boltzmann law.
		Stefan provided the first measurements of the thermal conductivity of gases, treated evaporation, and among others studied diffusion, heat conduction in fluids.
	encyclopedia.calendarhome.com /cgi-bin/encyclopedia.pl?p=Joseph_Stefan (678 words)

	Stefan-Boltzmann law - Definition, explanation
		The law was experimentally discovered by Jožef Stefan; (1835-1893) in 1879 and theoretically derived in the frame of the thermodynamics by Ludwig Boltzmann (1844-1906) in 1884.
		Stefan published this law on March 20 in the article Über die Beziehung zwischen der Wärmestrahlung und der Temperatur (On the relationship between thermal radiation and temperature) in the Bulletins from the sessions of the Vienna Academy of Sciences.
		The Stefan-Boltzmann law can be easily derived by integrating the emitted intensity from the surface of a fl body given by Planck's law of fl body radiation over the half-sphere into which it is emitted, and over all frequencies.
	www.calsky.com /lexikon/en/txt/s/st/stefan_boltzmann_law.php (839 words)

	eFunda: Theory of Pyrometers
		The Stefan-Boltzmann law is used in broad-band pyrometers, where a wide range of wavelengths are measured.
		The radiation intensity and wavelength from a flbody at a given temperature T is governed by Planck's law.
		Planck's law and the Stefan-Boltzmann law are derived assuming flbody properties.
	www.efunda.com /designstandards/sensors/pyrometers/pyrometers_theory.cfm (562 words)

	Joseph Stefan (1835-1893)
		Joseph Stefan was in 1835 in St. Peter and died in Vienna in 1893.
		Stefan's based his studies on Maxwell's equations in 1879.
		His student in Vienna, Ludwig Boltzmann derived it from statistical mechanics in 1884.
	rclsgi.eng.ohio-state.edu /courses/Korpela/images/htransfer/stefan.html (103 words)

	JHT History of Heat Transfer - Stefan (Site not responding. Last check: )
		Stefan was educated at the University of Wien, received his Doctor of Philosophy in 1858 and became Privatdozent in Mathematical Physics.
		Stefan showed empirically in 1879 that the radiation of such a body was proportional to the fourth power of its absolute temperatures.
		In the year 1891, Stefan published his work on the formation of ice in the Polar Seas, giving a special solution of this non-linear conduction problem with phase change (the more general solution being due to F. Neumann).
	www.me.utexas.edu /~me339/Bios/stefan.html (211 words)

	BOLTZMANN, Ludwig (Site not responding. Last check: )
		A professor of physics at various German and Austrian universities for more than 40 years, Boltzmann first demonstrated the law of thermal radiation, named for him and the Austrian physicist Josef Stefan (1835–93).
		The Stefan-Boltzmann law states that the total radiation from a flbody, which is an ideal body or surface that absorbs all radiant energy and reflects none, is proportional to the fourth power of the absolute temperature of the flbody.
		Boltzmann also made an important contribution to the field of thermodynamics with his studies of the movements of gas molecules.
	www.history.com /encyclopedia.do?articleId=203334 (235 words)

	Josef Stefan (Site not responding. Last check: )
		Josef Stefan was appointed lecturer in mathematical physics at Vienna in 1858 and became a professor there in 1866.
		Boltzmann, one of his students, showed in 1884 that this Stefan-Boltzmann law could be demonstrated mathematically.
		Stefan then applied it to determine the approximate temperature of the surface of the Sun.
	physics.rug.ac.be /Fysica/Geschiedenis/Mathematicians/Stefan.html (107 words)

	Stefan-Boltzmann constant Summary
		The main conclusion from Boltzmann's work with gasses is that entropy is a measure of the probability of a state; that is, apart from an additive constant, the entropy is proportional to the log of the probability of the thermodynamic state.
		Boltzmann's constant, often referred to as the gas constant per molecule, can be substituted for R/NA which yields PV = NkT, where P is pressure, V volume, N the number of molecules, k Boltzmann's constant, and T temperature.
		The Stefan-Boltzmann constant (also Stefan's constant), a physical constant denoted by the Greek letter σ, is the constant of proportionality in the Stefan-Boltzmann law: the total energy radiated per unit surface area of a fl body in unit time is proportional to the fourth power of the thermodynamic temperature.
	www.bookrags.com /Stefan-Boltzmann_constant (589 words)

	Mars Climate Modeling
		Wien's Law relates the wavelength of the point of maximum intensity in the continuous spectrum of a fl body inversely proportional to the body's absolute temperature.
		Kepler's Second Law states that the line joining the centers of mass of the sun and a planet covers an area that increases at a constant rate as the planet moves in its orbit (i.e.
		Kepler's Third Law states that the square of the sidereal period divided by the cube of the planet's mean distance from the sun forms a ratio that is the same for all of the planets (i.e.
	physics.gmu.edu /~hgeller/marsclim.html (780 words)

	The laws list: S
		The constant of proportionality present in the Stefan-Boltzmann law.
		The radiated power P (rate of emission of electromagnetic energy) of a hot body is proportional to the radiating surface area, A, and the fourth power of the thermodynamic temperature, T.
		Laws, rules, principles, effects, paradoxes, limits, constants, experiments, and thought-experiments in physics.
	www.alcyone.com /max/physics/laws/s.html (993 words)

	Joseph Stefan Summary
		This law is used today by astronomers to determine the temperature of stars, the interstellar medium, and gases swirling into fl holes based solely on the wavelength of light emitted by these objects.
		Joseph Stefan (Slovene Jožef Stefan) (March 24, 1835 – January 7, 1893) was a Slovene-Austrian physicist, mathematician and poet.
		Stefan was born in an outskirt village St.
	www.bookrags.com /Joseph_Stefan (730 words)

	Stefan-Boltzmann law - Education - Information - Educational Resources - Encyclopedia - Music
		The law was experimentally discovered by Jožef Stefan (1835-1893) in 1879 and theoretically derived in the frame of the thermodynamics by Ludwig Boltzmann (1844-1906) in 1884.
		Boltzmann treated a certain ideal heat engine with the light as a working matter instead of the gas.
		Stefan published this law on March 20 in the article Über die Beziehung zwischen der Wärmestrahlung und der Temperatur (On the relationship between thermal radiation and temperature) in the Bulletins from the sessions of the Vienna Academy of Sciences.
	www.music.us /education/S/Stefan-Boltzmann-law.htm (932 words)

	Infrared Blackbody Theory
		If the surface is very rough, the wedges are deep, and the object will have radiating properties that are closer to those of a flbody than if the surface were smooth.
		It can be observed that as temperature increases, not only does the amount of radiation per unit area increase, but the wavelength at which the radiation is maximum shifts to shorter wavelengths.
		The value of the wavelength of maximum radiation per unit area is given by Wien’s Displacement Law.
	www.mikroninfrared.com /products/blackbody/about-blackbody.html (774 words)

	S
		As the theorems assume the laws of general relativity and certain general properties of matter, but nothing else, they are valid quite generally.
		In the context of general relativity: a solution or, more precisely, a solution of the Einstein equations is a model universe that follows the law of gravity as prescribed by general relativity.
		One of the laws governing the properties of the simplest form of thermal radiation - that emitted by a flbody: The total energy emitted by such a body is proportional to the fourth power of its temperature (measured in Kelvin).
	www.einstein-online.info /en/navMeta/dictionary/s/index.html (3351 words)

	8.5 Cosmic Engine
		Wien’s law indicates that as the temperature of a body increases, the wavelength at which maximum emission of radiation occurs is displaced toward lower wavelengths.
		This law states that the energy flux, F (in joules per square metre of surface per second), from a flbody is directly proportional to the fourth power of the object’s temperature, T (measured in Kelvin).
		Using Wien’s Law and photometric analysis of sunspots, the temperature of the center of a typical sunspot is found to be 4300 K (4).
	webs.mn.catholic.edu.au /physics/emery/prelim_cosmic.htm (10480 words)

	Stefan-Boltzmann Law
		I've been reading about the Stefan-Boltzmann law, but there is one thing that I don't understand.
		I remember some author expressed surprise that quantum mechanics got its start from the study of flbody radiation rather than some other phenomenon that would have allowed easier analysis, such as the photoelectric effect or specific heat or atomic spectra.
		His student, Ludwig Boltzmann, derived the 4th power of absolute temperature T relationship from radiation thermodynamics and electromagnetic waves.
	www.physicsforums.com /showthread.php?t=28232 (648 words)

	Imagine the Universe! Dictionary
		For a wavefront intersecting a reflecting surface, the angle of incidence is equal to the angle of reflection, in the same plane defined by the ray of incidence and the normal.
		The principle, employed by Einstein's relativity theories, that the laws of physics are the same, at least locally, in all coordinate frames.
		The constant of proportionality in Newton's law of universal gravitation and which plays an analogous role in A. Einstein's general relativity.
	imagine.gsfc.nasa.gov /docs/dict_qz.html (3025 words)

	Stefan-Boltzmann Law
		The energy radiated by a flbody radiator per second per unit area is proportional to the fourth power of the absolute temperature and is given by
		For ordinary temperatures (less than red hot"), the radiation is in the infrared region of the electromagnetic spectrum.
		The relationship governing radiation from hot objects is called the Stefan-Boltzmann law:
	hyperphysics.phy-astr.gsu.edu /hbase/thermo/stefan.html (252 words)

	The Stefan Boltzmann Law
		The behavior of flbody radiation is described by the Planck Law, but we can derive from the Planck Law two other radiation laws that are very useful: the Wien Displacement Law and the Stefan-Boltzmann Law.
		The Stefan-Boltzmann Law gives the total energy being emitted at all wavelengths by the flbody (which is the area under the Planck Law curve).
		Thus, the Stefan-Boltzmann Law explains the growth in the height of the curve as the temperature increases.
	csep10.phys.utk.edu /astr162/lect/light/radframe/sb_tl.html (102 words)

	Blackbody Radiation
		The Stefan-Boltzmann law predicts intensity output across varying wavelengths as a function of temperature.
		The second way is to move the peak wavelength by draggin on the graph itself.
		A simulation of the visible spectrum is displayed under the curve, corresponding to 400 (blue), 560 (green), and 700 (red) values.
	webphysics.davidson.edu /alumni/MiLee/java/bb_mjl.htm (221 words)

	Stefan-Boltzmann and Freezing Water
		One thing I did not notice, though, is the Stefan-Boltzmann law (radiative energy transfer being proportional to the fourth power of temperature).
		I am not a physicist and it has been a LONG time since my undergraduate physics days, but I do not know if the Stefan-Boltzmann law applies at relatively low temperatures like boiling water or if it only applies at stellar surface class temperatures.
		It was indelibly burned into my mind one incredibly embarrassing evening in a pool hall in my home town when I was home from my studies as a physics major at the University of Chicago.
	www.newton.dep.anl.gov /askasci/phy00/phy00750.htm (644 words)

	Stefan Boltzmann Law
		The filament temperatures can be determined by carefully measuring the voltage and current flowing through the lamp.
		From the Ohm's law you may find the resistance of the filament
		For small temperature changes the temperature of the tungsten filament can be calculated from the equation relating the change in the resistance to the increase of the temperature
	personal.tcu.edu /~zerda/manual/lab22.htm (880 words)

	Radiation Laws
		The primary law governing flbody radiation is the Planck Radiation Law, which governs the intensity of radiation emitted by unit surface area into a fixed direction from the flbody as a function of wavelength for a fixed temperature.
		The behavior of flbody radiation is described by the Planck Law, but we can derive from the Planck Law two other radiation laws that are very useful.
		The Wien Law gives the wavelength of the peak of the radiation distribution, while the Stefan-Boltzmann Law gives the total energy being emitted at all wavelengths by the flbody per unit time.
	www.pas.rochester.edu /~blackman/ast104/radiation.html (816 words)

	Radiation Laws \| Planck's Law \| Stefan-Boltzmann Law
		By differentiating Equation 1 (Planck's Law), it is possible to determine the wavelength of maximum radiation emission from the Sun:
		This is Wien's Law and for T = 5800K (the solar surface temperature) the wavelength of maximum energy is approximately 0.5
		Figure 1.2 shows the ideal solution to Planck's Law (Equation 1) for the spectrum of energy arriving at the top of the Earth's atmosphere.
	www.global-climate-change.org.uk /1-2-3.php (478 words)

	Temperature of the Early Earth
		The R-Squared law states that the farther you are from an emitting object, the less light you receive.
		The Law of Conservation of Energy tells us that the amount lost (in the infrared) has to equal the amount received (in the visible).
		The amount of sunlight falling on the Earth per square centimeter is given by multiplying the intensity at the Earth's orbit by the area cut out of the Sun's radiation beam by the Earth.
	www.globalchange.umich.edu /globalchange1/fall2004/lectures/energy_balance/early_earth.html (878 words)

	Thermal Sources
		Radiation laws govern the properties of the continuous spectrum.
		The primary law governing radiation is the Planck Radiation Law, which gives the intensity of radiation emitted by a flbody as a function of wavelength for a fixed temperature.
		The Wien law explains the shift of the peak to shorter wavelengths as the temperature increases, while the Stefan-Boltzmann law explains the growth in the height of the curve as the temperature increases.
	electron9.phys.utk.edu /optics421/modules/m4/sources.htm (682 words)

	Re: Exceptions to Newton's Law of Cooling
		Conduction is governed by Fourier's Law, which states that the rate of heat transfer is proportional to the temperature gradient (dT/dx) at any point in the solid.
		This is a whole subject in-and-of itself, and in fact I spent a whole semester in a graduate-level class on convection deriving the equations for the convective heat transfer coefficient for various cases.
		However, it is still useful to use the form of Newton's Law of Cooling, and thermodynamicists do this by simply dumping the extra deltaT^1/4 (for laminar flow) or deltaT^1/3 (for turbulent flow) into h.
	www.madsci.org /posts/archives/2005-08/1123680375.Ph.r.html (708 words)

	Unit 4
		The relationship between a star’s color, the shape of its continuum spectrum (i.e., where it peaks in wavelength), its absorption line spectrum, its spectral type, its surface temperature, and the amount of energy emitted from a unit area on the star’s surface is discussed.
		According to Planck’s Law a fl body emits a continuous spectrum as a function of wavelength.
		According to the laws of Quantum Mechanics, there are only a specific number of energy states in which a given atom, ion, or molecule can exist.
	www.phyast.pitt.edu /~hamilton/astro89/unit04.htm (939 words)

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