Articles on "Electricity" Why three prongs?Why do wall outlets have three holes? "Grounding" and safety. Right Angle CircuitryDo Lenz' Law and the Right Hand rule still work... after you've been turned INSIDE OUT by that greasy black Fog? "Static Electric" misconceptionsA list of things which gave me a warped view of Electrostatics. Speed of "Electricity"? Triboelectric Series If a cat gets trapped in a clothes dryer full of nylon pantyhose, which way do the electrons flow? Where does EM energy flow in a circuit? How Scientists Define the word "Electricity" Quotes from J.C. Barriers to Understanding ElectricityTwenty misconceptions which prevented me from understanding simple electrical science as a student. "Static" Electricity is really just high voltage.Scuff on the rug, then measure your body voltage. Electricity mistakes and 'nitpicking' also How SHOULD we teach Electricity? "Static" sparks Doorknob sparks and zapping yourself on the car door... and people who suffer from an "electric shock" disease.

Matrix mechanics Matrix mechanics is a formulation of quantum mechanics created by Werner Heisenberg, Max Born, and Pascual Jordan in 1925. Matrix mechanics was the first conceptually autonomous and logically consistent formulation of quantum mechanics. It extended the Bohr Model by describing how the quantum jumps occur. It did so by interpreting the physical properties of particles as matrices that evolve in time. It is equivalent to the Schrödinger wave formulation of quantum mechanics, and is the basis of Dirac's bra-ket notation for the wave function. Development of matrix mechanics In 1925, Werner Heisenberg, Max Born, and Pascual Jordan formulated the matrix mechanics representation of quantum mechanics. Epiphany at Helgoland In 1925 Werner Heisenberg was working in Göttingen on the problem of calculating the spectral lines of hydrogen. "It was about three o' clock at night when the final result of the calculation lay before me. The Three Papers Heisenberg's reasoning . Further discussion Nobel Prize

Physics | Main Richard Feynman is a hero of mine. If you like physics, you should get to know his work. You can find a list of Feynman resources here. A note on how I teach mechanics The kinematic equations are commonly presented and used in the mechanics portion of introductory physics courses. The problem I have with introducing them too early is that they lead to a rote approach to problem solving that in the end won't serve you well in your study of physics. Instead, I strongly suggest that you solve every problem as if you were "re-inventing the wheel" every time. Think about problems in the simplest terms: What is happening physically? You'll find that in no time, as you repeat similar kinds of problems and as you notice patterns, that you'll start to take shortcuts. All of the problems solved in problem sets and examples in this section are solved using this approach.

Dimensions Home A film for a wide audience! Nine chapters, two hours of maths, that take you gradually up to the fourth dimension. Mathematical vertigo guaranteed! Click on the image on the left to watch the trailer ! Free download and you can watch the films online! The film can also be ordered as a DVD. This film is being distributed under a Creative Commons license. Now with even more languages for the commentary and subtitles: Commentary in Arabic, English, French, German, Italian, Japanese, Spanish and Russian. Film produced by: Jos Leys (Graphics and animations) Étienne Ghys (Scenario and mathematics) Aurélien Alvarez (Realisation and post-production)

schoolphysics IoHT :: 110+ Variations of the Second Law of Thermodynamics Questions about these second law variations? Know of other second law definitions? Copyright © Institute of Human Thermodynamics and IoHT Publishing Ltd. All Rights Reserved [1] Hippocrates (c. 440 BC). [2] Lavoisier, A. (1789). [3-4] Carnot, S. (1824). [5-8] Clausius, R. (1850). [9] Kelvin, L. (1852). [10] Kelvin, L. (1852). [11] Kelvin, L. (1852). [12] Kelvin, L. (1852). [13] Kelvin, L. (1852). the Philosophical Magazine, October, 1852; also Mathematical and Physical Papers, vol. i, art. 59. [14] Clausius, R. (1865). [15] Kelvin & Planck. (1879). [16-17] Planck. [18] Caratheodory, C. (1908). [19-21] Fermi, E. (1936). [22-23] Bridgman, P. (1941). [24] Keenan, J. (1941). [25-26] Klotz. [27] Fritz, A. (1959). [28] King, A. (1962). [29-30] Lee, J. & Sears, F. (1963). [31-32] Bazarov, I. (1964). [33] Bent, H. (1965). [34] Hatsopoulos, G. & Keenan, J. (1965). [35-37] Kern, R. & Weisbrod, A. (1967). [38] Battino, R. & Wood, S. (1968). [39] Bekenstein, J. (1971). [40-41] Lehninger, A. (1971).

La Brachistocrona | Giocando con la Gravità | Fandom powered by Wikia Il problema della brachistocrona consiste nel trovare la particolare traiettoria che un corpo, soggetto alla sola forza peso, deve compiere nel passare da un punto ad un punto posto ad una quota più bassa, che sia tale da minimizzare il tempo di percorrenza. La ricerca di questa curva può avvenire notando l'analogia con quanto avviene per la rifrazione della luce. e si trovano agli estremi di due strati di materiali diversi e di uguale spessore h. e percorre i tratti con tempi di percorrenza . . Dove con abbiamo indicato gli angoli di incidenza e di rifrazione dispetto alla normale alla superficie di separazione. con una opportuna costante. Si può generalizzare questo risultato applicando più volte ad una successione di strati contigui di uguale spessore e di materiali diversi. al una velocità e resta determinato il punto di passaggio tra ciascuno strato. al punto è dato da: allora sarà tanto piccolo quanto più è piccolo e quindi se la velocità nel primo tratto tende a zero allora Sia costante L'angolo

Special Relativity Special Relativity These pages are ok as far as they go, but they are missing the planned highlight, to show you what things actually look like when you travel at near the speed of light. I hope to have the opportunity to develop these pages further as time permits. Here is my opinionated Guide to Special Relativistic Flight Simulator Sites. Meanwhile, these pages comprise an animated introduction to the elements of Special Relativity. And don't miss Prasenjit Saha's Interactive Lorentz Transformations. © 1998, 1999 Andrew Hamilton. Forward to The Postulates of Special Relativity Hey, get me back to Falling into a Black Hole Unless otherwise stated, clicking on images gives you enlarged versions thereof, which may be easier to view in a classroom environment. Special Relativity: Index Andrew Hamilton's Homepage Other Relativity and Black Hole links

Suprathreshold stochastic resonance Suprathreshold Stochastic Resonance (SSR) is a variant of stochastic resonance (SR) that occurs for a specific set of conditions that are somewhat different from those of stochastic resonance. Like stochastic resonance, suprathreshold stochastic resonance describes the observation of noise enhanced behaviour in signal processing systems. Unlike conventional stochastic resonance, suprathreshold stochastic resonance does not disappear when the signal is no longer "subthreshold." Introduction Suprathreshold stochastic resonance was first demonstrated in arrays of identical threshold devices in 2000. This initial work (Stocks 2000) assumed an aperiodic random input signal (meaning that suprathreshold stochastic resonance is a form of aperiodic stochastic resonance), and stochastic resonance was shown to occur in the Shannon average mutual information between the input and output of the array. Figure 1 shows a simple example that satisfies these properties. Key theoretical results Applications

Usenet Physics FAQ Version Date: March 2013 This list of answers to frequently asked questions in physics was created by Scott Chase in 1992. Its purpose was to provide good answers to questions that had been discussed often in the sci.physics and related Internet news groups. The articles in this FAQ are based on those discussions and on information from good reference sources. They were later maintained and enlarged by Michael Weiss and Philip Gibbs. Others who have written for the FAQ are credited at the top of the items they submitted, while many more who have made smaller contributions have been thanked privately. Most of the entries that you'll find here were written in the days when the Internet was brand new. So because of their age, the FAQ entries that you'll find here have a great deal of academic credibility—but they are not always perfect and complete. This document is copyright. General Physics Particle and Nuclear Physics Quantum Physics Relativity and Cosmology Speed of Light Special Relativity

Open Source Physics 10 Strange Things About The Universe Space The universe can be a very strange place. While groundbreaking ideas such as quantum theory, relativity and even the Earth going around the Sun might be commonly accepted now, science still continues to show that the universe contains things you might find it difficult to believe, and even more difficult to get your head around. Theoretically, the lowest temperature that can be achieved is absolute zero, exactly ? One of the properties of a negative-energy vacuum is that light actually travels faster in it than it does in a normal vacuum, something that may one day allow people to travel faster than the speed of light in a kind of negative-energy vacuum bubble. One prediction of Einstein’s theory of general relativity is that when a large object moves, it drags the space-time around it, causing nearby objects to be pulled along as well. Relativity of Simultaneity Since this extra dimension is so small, only tiny objects, such as particles, can move along it. Antimatter Retrocausality

The Physics Classroom Gravitational microlensing Gravitational microlensing is an astronomical phenomenon due to the gravitational lens effect. It can be used to detect objects ranging from the mass of a planet to the mass of a star, regardless of the light they emit. Typically, astronomers can only detect bright objects that emit lots of light (stars) or large objects that block background light (clouds of gas and dust). When a distant star or quasar gets sufficiently aligned with a massive compact foreground object, the bending of light due to its gravitational field, as discussed by Einstein in 1915, leads to two distorted unresolved images resulting in an observable magnification. Since microlensing observations do not rely on radiation received from the lens object, this effect therefore allows astronomers to study massive objects no matter how faint. Microlensing by an isolated object was first detected in 1989. How it works[edit] Microlensing is based on the gravitational lens effect. Observing microlensing[edit] History[edit] .