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Black hole From Wikipedia, the free encyclopedia Jump to: navigation, search For other uses, see Black hole (disambiguation). Page semi-protected Simulated view of a black hole in front of the Large Magellanic Cloud. The ratio between the black hole Schwarzschild radius and the observer distance to it is 1:9. Of note is the gravitational lensing effect known as an Einstein ring, which produces a set of two fairly bright and large but highly distorted images of the Cloud as compared to its actual angular size. General relativity G_{\mu \nu} + \Lambda g_{\mu \nu}= {8\pi G\over c^4} T_{\mu \nu} Einstein field equations Introduction Mathematical formulation Resources [show]Fundamental concepts Special relativity Equivalence principle World line · Riemannian geometry [hide]Phenomena Kepler problem · Lenses · Waves Frame-dragging · Geodetic effect Event horizon · Singularity Black hole [show]Equations Linearized Gravity Post-Newtonian formalism Einstein field equations Friedmann equations ADM formalism BSSN formalism [show]Advanced theories Kaluza–Klein Quantum gravity [show]Solutions Schwarzschild Reissner-Nordström · Gödel Kerr · Kerr-Newman Kasner · Taub-NUT · Milne · Robertson-Walker pp-wave [show]Scientists Einstein · Minkowski · Eddington Lemaître · Schwarzschild Robertson · Kerr · Friedman Chandrasekhar · Hawking · others v · d · e

A black hole is a region of space from which nothing, not even light, can escape. It is the result of the deformation of spacetime caused by a very compact mass. Around a black hole there is an undetectable surface which marks the point of no return. This surface is called an event horizon. It is called "black" because it absorbs all the light that hits it, reflecting nothing, just like a perfect black body in thermodynamics.[1] Quantum mechanics predicts that black holes also emit radiation like a black body with a finite temperature. This temperature decreases with the mass of the black hole, making it difficult to observe this radiation for black holes of stellar mass.

Despite its invisible interior, a black hole can be observed through its interaction with other matter. A black hole can be inferred by tracking the movement of a group of stars that orbit a region in space. Alternatively, when gas falls into a stellar black hole from a companion star, the gas spirals inward, heating to very high temperatures and emitting large amounts of radiation that can be detected from earthbound and Earth-orbiting telescopes.

Astronomers have identified numerous stellar black hole candidates, and have also found evidence of supermassive black holes at the center of galaxies. In 1998, astronomers found compelling evidence that a supermassive black hole of more than 2 million solar masses is located near the Sagittarius A* region in the center of the Milky Way galaxy. Recent results indicate that the supermassive black hole is more than 4 million solar masses. Contents [hide]

* 1 History o 1.1 General relativity