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| | My name's Will Schlenker but everybody calls me Will. I'm from Germany. I'm studying at the university (final year) and I play the Trombone for 7 years. Usually I choose songs from the famous films :D. <br>I have two sister. I like Videophilia (Home theater), watching TV (2 Broke Girls) and Chess.<br><br>Here is my page [http://dodge.surrey.bc.vintagecarnet.com/groups/how-to-get-free-fifa-15-coins-676910876/ FIFA 15 coin hack] |
| {{see also|history of special relativity}}
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| {{General relativity}}
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| [[General relativity]] (GR) is a [[theory of gravitation]] that was developed by [[Albert Einstein]] between 1907 and 1915, with contributions by many others after 1915. According to general relativity, the observed gravitational attraction between masses results from the warping of space and time by those masses.
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| Before the advent of general relativity, Newton's law of universal gravitation had been accepted for more than two hundred years as a valid description of the gravitational force between masses, even though Newton himself did not regard the theory as the final word on the nature of gravity. Within a century of Newton's formulation, careful astronomical observation revealed unexplainable variations between the theory and the observations. Under Newton's model, gravity was the result of an attractive force between massive objects. Although even Newton was bothered by the unknown nature of that force, the basic framework was extremely successful at describing motion.
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| However, experiments and observations show that Einstein's description accounts for several effects that are unexplained by Newton's law, such as minute anomalies in the orbits of Mercury and other planets. General relativity also predicts novel effects of gravity, such as gravitational waves, gravitational lensing and an effect of gravity on time known as gravitational time dilation. Many of these predictions have been confirmed by experiment, while others are the subject of ongoing research. For example, although there is indirect evidence for gravitational waves, direct evidence of their existence is still being sought by several teams of scientists in experiments such as the [[LIGO]] and [[GEO 600]] projects.
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| General relativity has developed into an essential tool in modern astrophysics. It provides the foundation for the current understanding of black holes, regions of space where gravitational attraction is so strong that not even light can escape. Their strong gravity is thought to be responsible for the intense radiation emitted by certain types of astronomical objects (such as active galactic nuclei or microquasars). General relativity is also part of the framework of the standard Big Bang model of cosmology.
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| ==Creation of general relativity==
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| === Early investigations ===
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| As Einstein later said, the reason for the development of general relativity was the preference of inertial motion within [[special relativity]], while a theory which from the outset prefers no state of motion (even accelerated ones) appeared more satisfactory to him.<ref>Albert Einstein, [http://nobelprize.org/nobel_prizes/physics/laureates/1921/einstein-lecture.html Nobel lecture] in 1921</ref> So, while still working at the patent office in 1907, Einstein had what he would call his "happiest thought". He realized that the principle of relativity could be extended to gravitational fields.
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| Consequently, in 1907 (published 1908) he wrote an article on acceleration under [[special relativity]].<ref>{{Citation|author= Einstein, A. | title= Relativitätsprinzip und die aus demselben gezogenen Folgerungen (On the Relativity Principle and the Conclusions Drawn from It)| journal= Jahrbuch der Radioaktivität (Yearbook of Radioactivity) | volume= 4|pages= 411–462}} page 454 (Wir betrachen zwei Bewegung systeme ...)</ref>
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| In that article, he argued that [[free fall]] is really inertial motion, and that for a freefalling observer the rules of special relativity must apply. This argument is called the [[Equivalence principle]]. In the same article, Einstein also predicted the phenomenon of [[gravitational time dilation]].
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| In 1911, Einstein published another article expanding on the 1907 article.<ref>{{Citation|last=Einstein |first=Albert |title=Einfluss der Schwerkraft auf die Ausbreitung des Lichtes (On the Influence of Gravity on the Propagation of Light) |journal=Annalen der Physik |year=1911 |volume=35 |pages=898–908 |doi=10.1002/andp.19113401005|bibcode = 1911AnP...340..898E }} (also in ''Collected Papers'' Vol. 3, document 23)</ref>
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| There, he thought about the case of a uniformly accelerated box not in a gravitational field, and noted that it would be indistinguishable from a box sitting still in an unchanging gravitational field. He used special relativity to see that the rate of clocks at the top of a box accelerating upward would be faster than the rate of clocks at the bottom. He concludes that the rates of clocks depend on their position in a gravitational field, and that the difference in rate is proportional to the gravitational potential to first approximation.
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| Also the [[Gravitational lensing|deflection of light]] by massive bodies was predicted. Although the approximation was crude, it allowed him to calculate that the deflection is nonzero. German astronomer [[Erwin Finlay-Freundlich]] publicized Einstein's challenge to scientists around the world.<ref name="Crelinston_1">Crelinsten, Jeffrey. "[http://www.pupress.princeton.edu/titles/8165.html Einstein's Jury: The Race to Test Relativity]". ''[[Princeton University Press]].'' 2006. Retrieved on 13 March 2007. ISBN 978-0-691-12310-3</ref> This urged astronomers to detect the deflection of light during a [[solar eclipse]], and gave Einstein confidence that the scalar theory of gravity proposed by [[Gunnar Nordström]] was incorrect. But the actual value for the deflection that he calculated was too small by a factor of two, because the approximation he used doesn't work well for things moving at near the speed of light. When Einstein finished the full theory of general relativity, he would rectify this error and predict the correct amount of light deflection by the sun.
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| Another of Einstein's notable thought experiments about the nature of the gravitational field is that of the rotating disk (a variant of the [[Ehrenfest paradox]]). He imagined an observer making experiments on a rotating turntable. He noted that such an observer would find a different value for the mathematical constant π than the one predicted by Euclidean geometry. The reason is that the radius of a circle would be measured with an uncontracted ruler, but, according to special relativity, the circumference would seem to be longer because the ruler would be contracted. Since Einstein believed that the laws of physics were local, described by local fields, he concluded from this that spacetime could be locally curved. This led him to study [[Riemannian geometry]], and to formulate general relativity in this language.
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| ===Developing general relativity===
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| [[File:1919 eclipse positive.jpg|alt=Black circle covering the sun, rays visible around it, in a dark sky.|left|thumb|upright|[[Arthur Stanley Eddington|Eddington]]'s photograph of a solar eclipse, which confirmed Einstein's theory that light "bends".]]
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| In 1912, Einstein returned to Switzerland to accept a professorship at his ''alma mater'', the ETH. Once back in Zurich, he immediately visited his old ETH classmate [[Marcel Grossmann]], now a professor of mathematics, who introduced him to Riemannian geometry and, more generally, to [[differential geometry]]. On the recommendation of Italian mathematician [[Tullio Levi-Civita]], Einstein began exploring the usefulness of [[general covariance]] (essentially the use of [[tensor]]s) for his gravitational theory. For a while Einstein thought that there were problems with the approach, but he later returned to it and, by late 1915, had published his [[general theory of relativity]] in the form in which it is used today.<ref>{{Harv|Einstein|1915}}</ref> This theory explains gravitation as distortion of the structure of [[spacetime]] by matter, affecting the [[inertia]]l motion of other matter.
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| During World War I, the work of [[Central Powers]] scientists was available only to Central Powers academics, for national security reasons. Some of Einstein's work did reach the United Kingdom and the United States through the efforts of the Austrian [[Paul Ehrenfest]] and physicists in the Netherlands, especially 1902 Nobel Prize-winner [[Hendrik Lorentz]] and [[Willem de Sitter]] of [[Leiden University]]. After the war ended, Einstein maintained his relationship with Leiden University, accepting a contract as an ''[[Professor#Netherlands|Extraordinary Professor]]''; for ten years, from 1920 to 1930, he travelled to Holland regularly to lecture.<ref>{{Citation|url=http://www.lorentz.leidenuniv.nl/history/einstein/einstein.html|title=Two friends in Leiden|accessdate=11 June 2007}}</ref>
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| In 1917, several astronomers accepted Einstein 's 1911 challenge from Prague. The [[Mount Wilson Observatory]] in California, U.S., published a solar [[spectroscopic]] analysis that showed no gravitational redshift.<ref>{{Citation|last =Crelinsten |first =Jeffrey |title =Einstein's Jury: The Race to Test Relativity |isbn =978-0-691-12310-3 |publisher =Princeton University Press |pages = 103–108 |year =2006 |url =http://www.pupress.princeton.edu/titles/8165.html |accessdate =13 March 2007 |ref =}}</ref> In 1918, the [[Lick Observatory]], also in California, announced that it too had disproved Einstein's prediction, although its findings were not published.<ref>{{Citation|last =Crelinsten |first =Jeffrey |title =Einstein's Jury: The Race to Test Relativity |isbn =978-0-691-12310-3 |publisher =Princeton University Press |pages = 114–119 |year =2006 |url =http://www.pupress.princeton.edu/titles/8165.html |accessdate =13 March 2007 }}</ref>
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| However, in May 1919, a team led by the British astronomer [[Arthur Stanley Eddington]] claimed to have confirmed Einstein's prediction of [[gravitational lensing|gravitational deflection of starlight]] by the Sun while photographing a solar eclipse with dual expeditions in [[Sobral, Ceará|Sobral]], northern [[Brazil]], and [[Príncipe]], a west African island.<ref name="Crelinston_1"/> Nobel laureate [[Max Born]] praised general relativity as the "greatest feat of human thinking about nature";<ref>{{Citation |title = The genius of space and time
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| |url = http://books.guardian.co.uk/reviews/scienceandnature/0,,1571826,00.html |publisher = The Guardian |date = 17 September 2005 |accessdate = 31 March 2007 | location=London | first=PD | last=Smith}}</ref> fellow laureate [[Paul Dirac]] was quoted saying it was "probably the greatest scientific discovery ever made".<ref name="schmidhuber">[[Jürgen Schmidhuber]]. "[http://www.idsia.ch/~juergen/einstein.html Albert Einstein (1879–1955) and the 'Greatest Scientific Discovery Ever']". 2006. Retrieved on 4 October 2006.</ref>
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| The international media guaranteed Einstein's global renown.
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| There have been claims that scrutiny of the specific photographs taken on the Eddington expedition showed the experimental uncertainty to be comparable to the same magnitude as the effect Eddington claimed to have demonstrated, and that a 1962 British expedition concluded that the method was inherently unreliable.<ref name="Eddington">{{Citation|last = Andrzej |first = Stasiak |year = 2003 |title = Myths in science |journal = EMBO Reports |volume = 4 |issue = 3 |page = 236|doi =10.1038/sj.embor.embor779 |url = http://www.nature.com/embor/journal/v4/n3/full/embor779.html |accessdate = 31 March 2007}}</ref> The deflection of light during a solar eclipse was confirmed by later, more accurate observations.<ref>See the table in MathPages [http://www.mathpages.com/rr/s6-03/6-03.htm Bending Light]</ref> Some resented the newcomer's fame, notably among some German physicists, who later started the ''[[Deutsche Physik]]'' (German Physics) movement.<ref name="Hentschel">{{Citation |last = Hentschel |first = Klaus and Ann M. |year = 1996 |title = Physics and National Socialism: An Anthology of Primary Sources |pages = xxi |publisher = Birkhaeuser Verlag |isbn = 3-7643-5312-0 |nopp = true}}</ref><ref>For a discussion of astronomers' attitudes and debates about relativity, see {{Citation|last = Crelinsten |first = Jeffrey |title = Einstein's Jury: The Race to Test Relativity |publisher = Princeton University Press |year = 2006 |isbn = 0-691-12310-1}}, especially chapters 6, 9, 10 and 11.</ref>
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| ===General covariance and the hole argument===
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| By 1912, Einstein was actively seeking a theory in which [[gravitation]] was explained as a [[geometric]] phenomenon. At the urging of [[Tullio Levi-Civita]], Einstein began by exploring the use of [[general covariance]] (which is essentially the use of curvature [[tensors]]) to create a gravitational theory. However, in 1913 Einstein abandoned that approach, arguing that it is inconsistent based on the "[[hole argument]]". In 1914 and much of 1915, Einstein was trying to create [[field equations]] based on another approach. When that approach was proven to be inconsistent, Einstein revisited the concept of general covariance and discovered that the hole argument was flawed.
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| ===The development of the Einstein field equations===
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| {{main|Einstein field equations}}
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| When Einstein realized that general covariance was actually tenable, he quickly completed the development of the field equations that are named after him. However, he made a now-famous mistake. The field equations he published in October 1915 were
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| :<math>R_{\mu\nu} = T_{\mu\nu}\,</math>,
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| where <math>R_{\mu\nu}</math> is the [[Ricci tensor]], and <math>T_{\mu\nu}</math> the [[energy-momentum tensor]]. This predicted the non-[[Classical mechanics|Newtonian]] [[perihelion precession]] of [[Mercury (planet)|Mercury]], and so had Einstein very excited. However, it was soon realized that they were inconsistent with the local [[conservation of energy-momentum]] unless the universe had a constant density of mass-energy-momentum. In other words, air, rock and even a vacuum should all have the same density. This inconsistency with observation sent Einstein back to the drawing board. However, the solution was all but obvious, and in November 1915 Einstein published the actual Einstein field equations:
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| :<math>R_{\mu\nu} - {1\over 2}R g_{\mu\nu} = T_{\mu\nu}</math>,
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| where <math>R</math> is the [[Ricci scalar]] and <math>g_{\mu\nu}</math> the [[metric tensor]]. With the publication of the field equations, the issue became one of solving them for various cases and interpreting the solutions. This and experimental verification have dominated general relativity research ever since.
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| ===Einstein and Hilbert===
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| {{See also|Relativity priority dispute}}
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| Although Einstein is credited with finding the field equations, the German mathematician [[David Hilbert]] published them in an article before Einstein's article. This has resulted in accusations of [[plagiarism]] against Einstein (never from Hilbert), and assertions that the field equations should be called the "Einstein-Hilbert field equations". However, Hilbert did not press his claim for priority and some{{Who|date=October 2010}} have asserted that Einstein submitted the correct equations before Hilbert amended his own work to include them. This suggests that Einstein developed the correct field equations first, though Hilbert may have reached them later independently (or even learned of them afterwards through his correspondence with Einstein).<ref>Leo Corry, Jürgen Renn, John Stachel: "Belated Decision in the Hilbert-Einstein Priority Dispute", SCIENCE, Vol. 278, 14 November 1997 - [http://www.tau.ac.il/~corry/publications/articles/science.html article text]</ref> However, others have criticized those assertions.<ref>[http://physics.unr.edu/faculty/winterberg/Hilbert-Einstein.pdf Friedwart Winterberg's response to the Cory-Renn-Stachel paper] as printed in "Zeitschrift für Naturforschung" [http://www.znaturforsch.com/c59a.htm 59a], 715-719.</ref>
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| ===Sir Arthur Eddington===
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| In the early years after Einstein's theory was published, [[Arthur Eddington|Sir Arthur Eddington]] lent his considerable prestige in the British scientific establishment in an effort to champion the work of this German scientist. Because the theory was so complex and abstruse (even today it is popularly considered the pinnacle of scientific thinking; in the early years it was even more so), it was rumored that only three people in the world understood it. There was an illuminating, though probably apocryphal, anecdote about this. As related by [[Ludwik Silberstein]],<ref>John Waller (2002), ''Einstein's Luck'', Oxford University Press, ISBN 0-19-860719-9</ref> during one of Eddington's lectures he asked "Professor Eddington, you must be one of three persons in the world who understands general relativity." Eddington paused, unable to answer. Silberstein continued "Don't be modest, Eddington!" Finally, Eddington replied "On the contrary, I'm trying to think who the third person is."
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| ==Solutions==
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| === The Schwarzschild solution ===
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| Since the field equations are [[non-linear]], Einstein assumed that they were unsolvable. However, in 1915 [[Karl Schwarzschild]] discovered an exact solution for the case of a spherically symmetric [[spacetime]] surrounding a massive object in [[spherical coordinates]]. This is now known as the [[Schwarzschild solution]]. Since then, many other exact solutions have been found.
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| ===The expanding universe and the cosmological constant===
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| {{main|Cosmological constant}}
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| In 1922, [[Alexander Friedmann]] found a solution in which the universe may expand or contract, and later [[Georges Lemaître]] derived a solution for an expanding universe. However, Einstein believed that the universe was apparently static, and since a static cosmology was not supported by the general relativistic field equations, he added a [[cosmological constant]] Λ to the field equations, which became
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| :<math>R_{\mu\nu} - {1\over 2}R g_{\mu\nu} + \Lambda g_{\mu\nu} = T_{\mu\nu}</math>.
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| This permitted the creation of steady-state solutions, but they were unstable: the slightest perturbation of a static state would result in the universe expanding or contracting. In 1929, [[Edwin Hubble]] found evidence for the idea that the universe is expanding. This resulted in Einstein dropping the cosmological constant, referring to it as "the biggest blunder in my career". At the time, it was an [[ad hoc]] hypothesis to add in the cosmological constant, as it was only intended to justify one result (a static universe).
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| ===More exact solutions===
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| Progress in solving the field equations and understanding the solutions has been ongoing. The solution for a spherically symmetric charged object was discovered by Reissner and later rediscovered by Nordström, and is called the [[Reissner-Nordström black hole|Reissner-Nordström solution]]. The black hole aspect of the Schwarzschild solution was very controversial, and Einstein did not believe that singularities could be real. However, in 1957 (two years after Einstein's death in 1955), [[Martin Kruskal]] published a proof that black holes are called for by the Schwarzschild Solution. Additionally, the solution for a rotating massive object was obtained by [[Roy Kerr|Kerr]] in the 1960s and is called the [[Kerr solution]]. The [[Kerr-Newman solution]] for a rotating, charged massive object was published a few years later.
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| ==Testing the theory==
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| {{Main|Tests of general relativity}}
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| The perihelion precession of Mercury was the first evidence that general relativity is correct. Sir [[Arthur Stanley Eddington]]'s 1919 expedition in which he confirmed Einstein's prediction for the deflection of light by the Sun during the total [[solar eclipse of 29 May 1919]] helped to cement the status of general relativity as a likely true theory. Since then many observations have confirmed the correctness of general relativity. These include studies of [[binary pulsar]]s, observations of radio signals passing the limb of the Sun, and even the [[GPS]] system.
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| ==Alternative theories==
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| {{Main|Alternatives to general relativity}}
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| There have been various attempts to find modifications to general relativity. The most famous of these are the [[Brans-Dicke theory]] (also known as [[scalar-tensor theory]]), and [[Rosen's bimetric theory]]. Both of these theories proposed changes to the field equations of general relativity, and both suffer from these changes permitting the presence of bipolar gravitational radiation. As a result, Rosen's original theory has been refuted by observations of binary pulsars. As for Brans-Dicke (which has a tunable parameter ''ω'' such that ''ω = ∞'' is the same as general relativity), the amount by which it can differ from general relativity has been severely constrained by these observations.
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| In addition, general relativity is inconsistent with [[quantum mechanics]], the physical theory that describes the wave-particle duality of matter, and quantum mechanics does not currently describe gravitational attraction at relevant (microscopic) scales. There is a great deal of speculation in the physics community as to the modifications that might be needed to both general relativity and quantum mechanics in order to unite them consistently. The speculative theory that unites general relativity and quantum mechanics is usually called [[quantum gravity]], prominent examples of which include [[String Theory]] and [[Loop Quantum Gravity]].
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| ==More about GR history==
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| {{Unreferenced section|date=November 2010}}
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| {{Cleanup|section|Wikipedia is not a list or repository. This section needs to be rewritten in prose. Furthermore, a portion of the material below might be redundant, and already in other articles, and may not be relevant here.|date=October 2010}}
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| Kip Thorne identifies the "golden age of general relativity" as the period roughly from 1960 to 1975 during which the study of [[general relativity]],<ref>{{cite book |title=The future of theoretical physics and cosmology: celebrating Stephen Hawking's 60th birthday |chapter=Warping spacetime |first1=Kip |last1=Thorne |publisher=Cambridge University Press |year=2003 |isbn=0-521-82081-2 |page=74 |url=http://books.google.com/books?id=yLy4b61rfPwC}}, [http://books.google.com/books?id=yLy4b61rfPwC&pg=PA74 Extract of page 74]</ref> which had previously been regarded as something of a curiosity, entered the mainstream of [[theoretical physics]]. During this period, many of the concepts and terms which continue to inspire the imagination of gravitation researchers and the general public were introduced, including [[black hole]]s and '[[gravitational singularity]]'. At the same time, in a closely related development, the study of [[physical cosmology]] entered the mainstream and the [[Big Bang]] became well established. Areas of research included:
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| *The role of curvature in general relativity;
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| *The theoretical importance of black holes;
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| *The importance of geometrical machinery and levels of mathematical structure, especially [[local spacetime structure|local]] versus [[global spacetime structure]];
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| *The formulation of a competitor to general relativity (the Brans-Dicke theory);
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| *The first "precision tests" of gravitation theories.
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| Discoveries in observational astronomy included:
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| *[[Quasar]]s (objects the size of the [[solar system]] and as luminous as a hundred modern [[galaxy|galaxies]], so distant that they date from the early years of the universe);
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| *[[Pulsar]]s (soon interpreted as spinning [[neutron stars]]);
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| *The first credible candidate black hole, [[Cygnus X-1]];
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| *The [[cosmic background radiation]], hard evidence of the Big Bang and the subsequent expansion of the universe.
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| <!-- I don't know what this is, it doesn't seem to fit with the rest of the article so I'm commenting it out until someone can look through it.
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| '''Constellation of Sagittarius''', in the direction of the center of the galaxy.
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| That center- building up and out of the galactic disk- is tightly packed with stars.
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| regions of this so- called "bluge" the first to take notice was the physicist Karl Jansky back in the 1930s.He was asked by his employer, Bell Telephone Labs, to investigate sources of static that might interfere with what it saw as sthe killer app of its time... radio voice transmissions. Using this ungainly radio receiver... jansky methodically scanned the airwaves. he documented Thunderstorms, near and far and another sinal he could not
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| explain. It sounded like steam- a hiss of radio noise. Jansky narrowed it to a spot in the constellation of Sagittarius, in the direction of the center of the galaxy.Located within a larger pattern of radio emissions So Jansky's sighting would become known as Sagittarius A*. It was the 1960s and astronomy, like society was in a period of ferment. Startling new observation was being made and new interpretations were in the air. Quasars had just been discovered. Extremely bright beacons of light from deep space. Were they comming from the centers of distant galaxies? To study an event at the center of a galaxy, you have locate it. Young Becklin first took aim at our neighboring galaxy, Anedromeda. In ultravioled light, you can see a dense glow in the middle. Becklin found the point where the light reaches peak intensity and marked it as the Center. From our orientation in space, the entire Andromeda galaxy is in full view. But our galaxy is a different story. We live inside it, of course. Becklin had to find a way to see through all the dust and gas that obscure our line of sight into the center. So he went to a military contractor and obtained a device that reads infrared light, whose wavelengths are similar to the distances between particles in a dust cloud, allowing them to move right through. Becklin began measuring the brightness of the light as it rose to a peak, marking the location of the galactic center. Pinpointing this site would now allow astronomers to begin probing for details with a new generation of powerful telescopes, to peer into the bright lights. the forbidden zones, deep in the heart of the Milky Way. A few years later, in 1993, high atop Hawaii's Mauna Kea volcano. There were many problems, The American and German groups shared the same goal. to pinpoint the precise location of Sagittarius A*, and find out what it is. Because the object is too small to see at 26,000 light years away they would study it by tracking the orbits of starts around it. They tracked gas whipping around its center, figuring its speed at three million miles per hour, which led them to calculated the mass of whatever occupied M87's center at some 4 billion times that of our Sun. Their measurement- First-ever of its kind point to the presence of a Black Hole of truly super massive proportions. Searching Center, in search of clues to the origins and evolution of our galaxy. The Chandra X-ray space observatory recorded high energy radiation mostly likely given off by Ultra-dense neutron stars and small black holes. 20, 0000 black holes inhabit the inner three light years of the galactic center. In the last no other single object is known to weigh that much, its strong evidence of but it's still not iron clad proof.
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| by ''''Abdul Mughni Khan'''' -->
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| ==See also==
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| *[[Contributors to general relativity]]
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| *[[Golden age of physics]]
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| *[[Golden age of cosmology]]
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| ==Notes==
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| <references/>
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| ==References==
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| {{Wikisource|The Foundation of the Generalised Theory of Relativity}}
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| *{{cite book | author=Pais, Abraham | title= Subtle is the lord: the science and life of Albert Einstein| location=Oxford | publisher=Oxford University Press | year=1982 | isbn=0-19-853907-X}}
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| * {{cite journal | last1 = Einstein | first1 = A. | authorlink2 = Marcel Grossmann | last2 = Grossmann | first2 = M. | year = 1913 | title = Entwurf einer verallgemeinerten Relativitätstheorie und einer Theorie der Gravitation |trans_title = Outline of a Generalized Theory of Relativity and of a Theory of Gravitation | url = | journal = Zeitschrift für Mathematik und Physik | volume = 62 | issue = | pages = 225–261 }}
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| *''Einstein and the Changing Worldviews of Physics'' (editors—Lehner C., Renn J., Schemmel M.) 2012 ([[Birkhäuser]]).
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| * [http://www.bun.kyoto-u.ac.jp/~suchii/gen.GR.html Genesis of general relativity series]
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| [[Category:General relativity| ]]
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| [[Category:History of physics|General relativity]]
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| [[Category:Albert Einstein]]
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