Black hole

A black hole is a massive, compact <a href="/facts/Astronomical_object/BCHLa0Q2">astronomical object</a> so dense that its gravity prevents anything from escaping, even light. <a href="/facts/Albert_Einstein/CNTet8qu">Albert Einstein</a>'s theory of <a href="/facts/General_relativity/jVsoIg8X">general relativity</a> predicts that a sufficiently compact <a href="/facts/Mass/HHdc8XmF">mass</a> will form a black hole. The <a href="/facts/Boundary_(topology)/WgdH18kp">boundary</a> of no escape is called the <a href="/facts/Event_horizon/KXH2ptnI">event horizon</a>. A black hole has a great effect on the fate and circumstances of an object crossing it, but has no locally detectable features according to general relativity. In many ways, a black hole acts like an ideal <a href="/facts/Black_body/f0fHghDy">black body</a>, as it reflects no light. <a href="/facts/Quantum_field_theory_in_curved_spacetime/LF1ud943">Quantum field theory in curved spacetime</a> predicts that event horizons emit <a href="/facts/Hawking_radiation/J6R7W2wL">Hawking radiation</a>, with <a href="/facts/Thermal_radiation/1PD9jtCv">the same spectrum</a> as a black body of a <a href="/facts/Temperature/QyGe4gmj">temperature</a> inversely proportional to its mass. This temperature is of the <a href="/facts/Orders_of_magnitude_(temperature)/ADXGAk8e">order of billionths</a> of a <a href="/facts/Kelvin/E3trzC4C">kelvin</a> for <a href="/facts/Stellar_black_hole/8cz1uzAe">stellar black holes</a>, making it essentially impossible to observe directly.
Objects whose <a href="/facts/Gravitational_field/K1uTmJFy">gravitational fields</a> are too strong for light to escape were first considered in the 18th century by <a href="/facts/John_Michell/hoVarM2s">John Michell</a> and <a href="/facts/Pierre-Simon_Laplace/6ktp0txb">Pierre-Simon Laplace</a>. In 1916, <a href="/facts/Karl_Schwarzschild/u9KGeTey">Karl Schwarzschild</a> found the first modern solution of general relativity that would characterise a black hole. Due to his influential research, the <a href="/facts/Schwarzschild_metric/gkm25ScM">Schwarzschild metric</a> is named after him. <a href="/facts/David_Finkelstein/h6MDmTTF">David Finkelstein</a>, in 1958, first published the interpretation of "black hole" as a region of space from which nothing can escape. Black holes were long considered a mathematical curiosity; it was not until the 1960s that theoretical work showed they were a generic prediction of general relativity. The discovery of <a href="/facts/Neutron_star/4enfoxBA">neutron stars</a> by <a href="/facts/Jocelyn_Bell_Burnell/k81YuMlk">Jocelyn Bell Burnell</a> in 1967 sparked interest in <a href="/facts/Gravitationally_collapsed/7f4zQs8Y">gravitationally collapsed</a> compact objects as a possible astrophysical reality. The first black hole known was <a href="/facts/Cygnus_X-1/fv6UCHEU">Cygnus X-1</a>, identified by several researchers independently in 1971.
Black holes typically form when <a href="/facts/Stellar_evolution/Qa4vAGmn">massive stars collapse</a> at the end of their <a href="/facts/Stellar_evolution/Qa4vAGmn">life cycle</a>. After a black hole has formed, it can grow by absorbing mass from its surroundings. Supermassive black holes of millions of solar masses may form by absorbing other stars and merging with other black holes, or via <a href="/facts/Direct_collapse_black_hole/fUE1VvwK">direct collapse</a> of <a href="/facts/Gas_cloud/9eyVRraY">gas clouds</a>. There is consensus that <a href="/facts/Supermassive_black_hole/BcuTx8Q5">supermassive black holes</a> exist in the centres of most <a href="/facts/Galaxies/zCyUvEf7">galaxies</a>.
The presence of a black hole can be inferred through its interaction with other <a href="/facts/Matter/osyc04UN">matter</a> and with electromagnetic radiation such as visible light. Matter falling toward a black hole can form an <a href="/facts/Accretion_disk/8zJXshat">accretion disk</a> of infalling plasma, heated by <a href="/facts/Friction/d0108Rpu">friction</a> and emitting light. In extreme cases, this creates a <a href="/facts/Quasar/HS96328l">quasar</a>, some of the brightest objects in the universe. Stars passing too close to a supermassive black hole can be shredded into streamers that shine very brightly before being "swallowed." If other stars are orbiting a black hole, their orbits can be used to determine the black hole's mass and location. Such observations can be used to exclude possible alternatives such as <a href="/facts/Neutron_star/4enfoxBA">neutron stars</a>. In this way, astronomers have identified numerous stellar black hole candidates in <a href="/facts/Binary_star/TYlDe1bD">binary systems</a> and established that the radio source known as <a href="/facts/Sagittarius_A*/5TWIRfgm">Sagittarius A*</a>, at the core of the <a href="/facts/Milky_Way/ulF6lccN">Milky Way</a> galaxy, contains a supermassive black hole of about 4.3 million <a href="/facts/Solar_energy/YBSajyN4">solar</a> masses.

Black hole open-in-new

Black hole