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A binary black hole (BBH), or black hole binary, is a system consisting of two black holes in close orbit around each other. Like black holes themselves, binary black holes are often divided into binary stellar black holes , formed either as remnants of high-mass binary star systems or by dynamic processes and mutual capture; and binary ...
Final parsec problem: Supermassive black holes appear to have merged, and what appears to be a pair in this intermediate range has been observed, in PKS 1302–102. [23] However, theory predicts that when supermassive black holes reach a separation of about one parsec, it may take billions of years to orbit closely enough to merge—greater ...
One major problem lies in the mathematical framework of the Standard Model of physics, which is inconsistent with the theory of general relativity to the point that one or both theories break down under certain conditions (for example, within known spacetime singularities like the Big Bang and the centres of black holes beyond the event horizon ...
The second problem is that as the black holes move, one must continually adjust the location of the excision region to move with the black hole. The excision technique was developed over several years including the development of new gauge conditions that increased stability and work that demonstrated the ability of the excision regions to move ...
Astronomers said the V404 Cygni system holds a central black hole in the act of consuming a small star. This star appears to be very close to the black hole, orbiting it every 6.5 days, resembling ...
The Penrose process (also called Penrose mechanism) is theorised by Sir Roger Penrose as a means whereby energy can be extracted from a rotating black hole. [1] [2] [3] The process takes advantage of the ergosphere – a region of spacetime around the black hole dragged by its rotation faster than the speed of light, meaning that from the point of view of an outside observer any matter inside ...
In the membrane paradigm, the black hole is described as it should be seen by an array of these stationary, suspended noninertial observers, and since their shared coordinate system ends at the event horizon (because an observer cannot legally hover at or below the event horizon under general relativity), this conventional-looking radiation is ...
Euler's oblate three body problem and a Kerr black hole share the same mass moments, and this is most apparent if the metric for the latter is written in Kerr–Schild coordinates. The analogue of the oblate case augmented with a linear Hooke term is a Kerr–de Sitter black hole.