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• • • A black hole is a region of exhibiting such strong effects that nothing—not even and such as —can escape from inside it. The theory of predicts that a sufficiently compact can deform to form a black hole. The boundary of the region from which no escape is possible is called the. Although the event horizon has an enormous effect on the fate and circumstances of an object crossing it, no locally detectable features appear to be observed. In many ways a black hole acts like an ideal, as it reflects no light. Moreover, predicts that event horizons emit, with as a black body of a temperature inversely proportional to its mass. This temperature is on the order of billionths of a kelvin for, making it essentially impossible to observe.
Objects whose are too strong for light to escape were first considered in the 18th century. The first modern solution of general relativity that would characterize a black hole was found by in 1916, although its interpretation as a region of space from which nothing can escape was first published by in 1958. Black holes were long considered a mathematical curiosity; it was during the 1960s that theoretical work showed they were a generic prediction of general relativity. The discovery of by in 1967 sparked interest in compact objects as a possible astrophysical reality.
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Black holes of stellar mass are expected to form when very massive stars collapse at the end of their life cycle. After a black hole has formed, it can continue to grow by absorbing mass from its surroundings. By absorbing other stars and merging with other black holes, of millions of () may form. There is general consensus that supermassive black holes exist in the centers of most. Despite its invisible interior, the presence of a black hole can be inferred through its interaction with other and with such as visible light. Matter that falls onto a black hole can form an external heated by friction, forming some of the.
If there are other stars 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 neutron stars. In this way, astronomers have identified numerous stellar black hole candidates in, and established that the radio source known as, at the core of the galaxy, contains a supermassive black hole of about 4.3 million. On 11 February 2016, the collaboration of, which also represented the first observation of a black hole merger. As of December 2018, eleven have been observed that originated from ten merging black holes (along with one binary ). Simulated view of a black hole in front of the. Note the effect, which produces two enlarged but highly distorted views of the Cloud.
Across the top, the disk appears distorted into an arc. The idea of a body so massive that even light could not escape was briefly proposed by astronomical pioneer and English clergyman in a letter published in November 1784.
Michell's simplistic calculations assumed that such a body might have the same density as the Sun, and concluded that such a body would form when a star's diameter exceeds the Sun's by a factor of 500, and the surface exceeds the usual speed of light. Michell correctly noted that such supermassive but non-radiating bodies might be detectable through their gravitational effects on nearby visible bodies. Scholars of the time were initially excited by the proposal that giant but invisible stars might be hiding in plain view, but enthusiasm dampened when the wavelike nature of light became apparent in the early nineteenth century. If light were a wave rather than a ', it became unclear what, if any, influence gravity would have on escaping light waves.
Modern relativity discredits Michell's notion of a light ray shooting directly from the surface of a supermassive star, being slowed down by the star's gravity, stopping, and then free-falling back to the star's surface. General relativity In 1915, developed his theory of, having earlier shown that gravity does influence light's motion.