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List Of Fastest Rotating Black Holes
Below is a list of fastest rotating black holes measured in the dimensionless rotational parameter ''a''. Methodologies for spin measurements Accreting black hole spins can be measured by observing the X-ray spectrum of the black hole and identifying spectral features caused by certain characteristics of the accretion disc. This can be used to determine the innermost stable circular orbit and hence the spin. Another method measures the radiative efficiency of the accretion disc. List Prograde rotation See also * List of most massive black holes * Orders of magnitude (speed) To help compare different orders of magnitude, the following list describes various speed levels between approximately 2.2 m/s and 3.0 m/s (the speed of light). Values in bold are exact. List of orders of magnitude for speed See als ... References {{reflist, refs= {{Cite journal, last=Reynolds, first=Christopher S., date=29 November 2013, title=The spin of supermassive black holes, journ ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kerr
Kerr may refer to: People *Kerr (surname) *Kerr (given name) Places ;United States *Kerr Township, Champaign County, Illinois *Kerr, Montana, A US census-designated place *Kerr, Ohio, an unincorporated community *Kerr County, Texas Kerr County is a county located on the Edwards Plateau in the U.S. state of Texas. As of the 2020 census, its population was 52,598. Its county seat is Kerrville. The county was named by Joshua D. Brown for his fellow Kentucky native, Jam ... Other uses * KERR, A US radio station *Kerr, a brand of food Mason jars and lids * Clan Kerr, a Scottish clan See also * * * Ker (other) {{Disambiguation, geo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Accretion Disc
An accretion disk is a structure (often a circumstellar disk) formed by diffuse material in orbital motion around a massive central body. The central body is most frequently a star. Friction, uneven irradiance, magnetohydrodynamic effects, and other forces induce instabilities causing orbiting material in the disk to spiral inward toward the central body. Gravitational and frictional forces compress and raise the temperature of the material, causing the emission of electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and protostars radiate in the infrared; those around neutron stars and black holes in the X-ray part of the spectrum. The study of oscillation modes in accretion disks is referred to as diskoseismology. Manifestations Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Innermost Stable Circular Orbit
The innermost stable circular orbit (often called the ISCO) is the smallest marginally stable circular orbit in which a test particle can stably orbit a massive object in general relativity. The location of the ISCO, the ISCO-radius (r_), depends on the mass and angular momentum (spin) of the central object. The ISCO plays an important role in black hole accretion disks since it marks the inner edge of the disk. The ISCO should not be confused with the Roche limit, the innermost point where a physical object can orbit before tidal forces break it up. The ISCO is concerned with theoretical ''test particle''s, not real objects. In general terms, the ISCO will be far closer to the central object than the Roche limit. Basic concept In classical mechanics, an orbit is achieved when a test particle's angular momentum is enough to resist the gravity force of the central object. As the test particle approaches the central object, the required amount of angular momentum grows, due to the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Supermassive Black Hole
A supermassive black hole (SMBH or sometimes SBH) is the largest type of black hole, with its mass being on the order of hundreds of thousands, or millions to billions, of times the mass of the Sun (). Black holes are a class of astronomical objects that have undergone gravitational collapse, leaving behind spheroidal regions of space from which nothing can escape, including light. Observational evidence indicates that almost every large galaxy has a supermassive black hole at its center. For example, the Milky Way galaxy has a supermassive black hole at its center, corresponding to the radio source Sagittarius A*. Accretion of interstellar gas onto supermassive black holes is the process responsible for powering active galactic nuclei (AGNs) and quasars. Two supermassive black holes have been directly imaged by the Event Horizon Telescope: the black hole in the giant elliptical galaxy Messier 87 and the black hole at the Milky Way's center (Sagittarius A*). Descr ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
GRS 1915+105
GRS 1915+105 or V1487 Aquilae is an X-ray binary star system containing a main sequence star and a black hole. Transfer of material from the star to the black hole generates a relativistic jet, making this a microquasar system. The jet exhibits apparent superluminal motion. It was discovered on August 15, 1992 by the WATCH all-sky monitor aboard Granat. "GRS" stands for "GRANAT source", "1915" is the right ascension (19 hours and 15 minutes) and "105" reflects the approximate declination (10 degrees and 56 arcminutes). The near-infrared counterpart was determined by spectroscopic observations. The binary system lies 11,000 parsecs away in Aquila. The black hole in GRS 1915+105 is 10 to 18 solar masses. The black hole rotates at least 950 times per second, giving it a spin parameter >0.82 (1.0 is the theoretical maximum). Galactic superluminal source In 1994, GRS 1915+105 became the first known galactic source that ejects material with apparent superluminal motion ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
GX 339-4
GX 339-4 is a moderately strong variable galactic X-ray binary#Low-mass X-ray binary, low-mass X-ray binary (LMXB) source and black hole candidate that flares from time to time. From spectroscopic measurements, the mass of the black-hole was found to be at least of 5.8 solar masses. Thomas Henry Markert ''et al.'' discovered GX 339-4 in 1973, in data obtained by the Massachusetts Institute of Technology, MIT Cosmic Ray Experiment on OSO-7. An optical counterpoint to the X-ray source was found by Jonathan E. Grindlay in 1979, and it is optically variable star, variable. For that reason it was given a variable star designation, V821 Arae, in 1981. During the outbursts GX 339-4 shows evolution of quasi-periodic oscillations (QPOs). In the rising phase the QPO frequency monotonically increase as the CENBOL propagates closer to the black hole and in the declining phase the QPO frequency monotonically decreases since the CENBOL recedes away from the black hole after viscosity is ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
