726:. The center of gravity can add over 1000 km/s of kick velocity. The greatest kick velocities (approaching 5000 km/s) occur for equal-mass and equal-spin-magnitude black-hole binaries, when the spins directions are optimally oriented to be counter-aligned, parallel to the orbital plane or nearly aligned with the orbital angular momentum. This is enough to escape large galaxies. With more likely orientations, a smaller effect takes place, perhaps only a few hundred kilometers per second. This sort of speed can eject merging binary black holes from globular clusters, thus preventing the formation of massive black holes in globular-cluster cores. This, in turn, reduces the chances of subsequent mergers, and thus the chance of detecting gravitational waves. For non-spinning black holes a maximum recoil velocity of 175 km/s occurs for masses in the ratio of five to one. When spins are aligned in the orbital plane, a recoil of 5000 km/s is possible with two identical black holes. Parameters that may be of interest include the point at which the black holes merge, the mass ratio that produces maximum kick, and how much mass/energy is radiated via gravitational waves. In a head-on collision this fraction is calculated at 0.002, or 0.2%. One of the best candidates of the recoiled supermassive black holes is CXO J101527.2+625911.
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114:. As the orbiting black holes give off these waves, the orbit decays, and the orbital period decreases. This stage is called binary black hole inspiral. The black holes will merge once they are close enough. Once merged, the single hole settles down to a stable form, via a stage called ringdown, where any distortion in the shape is dissipated as more gravitational waves. In the final fraction of a second the black holes can reach extremely high velocity, and the gravitational wave amplitude reaches its peak.
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308:, a gradually shrinking orbit. The first stages of the inspiral take a very long time, as the gravitational waves emitted are very weak when the black holes are distant from each other. In addition to the orbit shrinking due to the emission of gravitational waves, extra angular momentum may be lost due to interactions with other matter present, such as other stars.
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110:. Therefore, during the late 20th and early 21st century, binary black holes became of great interest scientifically as a potential source of such waves and a means by which gravitational waves could be proven to exist. Binary black hole mergers would be one of the strongest known sources of gravitational waves in the universe, and thus offer a good chance of
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1443:; Yan, Renbin; Barmby, P.; Coil, Alison L.; Conselice, Christopher J.; Ivison, R. J.; Lin, Lihwai; Koo, David C.; Nandra, Kirpal; Salim, Samir; Small, Todd; Weiner, Benjamin J.; Cooper, Michael C.; Davis, Marc; Faber, S. M.; Guhathakurta, Puragra; et al. (6 April 2007). "The DEEP2 Galaxy Redshift Survey: AEGIS Observations of a Dual AGN at
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346:. In this region most of the emitted gravitational waves go towards the event horizon, and the amplitude of those escaping reduces. Remotely detected gravitational waves have an oscillation with fast-reducing amplitude, as echos of the merger event result from tighter and tighter spirals around the resulting black hole.
31:
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In the full calculations of an entire merger, several of the above methods can be used together. It is then important to fit the different pieces of the model that were worked out using different algorithms. The
Lazarus Project linked the parts on a spacelike hypersurface at the time of the merger.
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In numerical models, test geodesics are inserted to see whether they encounter an event horizon. As two black holes approach each other, a "duckbill" shape protrudes from each of the two event horizons towards the other one. This protrusion extends longer and narrower until it meets the protrusion
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simulations. Numerical relativity models space-time and simulates its change over time. In these calculations it is important to have enough fine detail close into the black holes, and yet have enough volume to determine the gravitation radiation that propagates to infinity. In order to reduce the
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Numerical-relativity techniques steadily improved from the initial attempts in the 1960s and 1970s. Long-term simulations of orbiting black holes, however, were not possible until three groups independently developed groundbreaking new methods to model the inspiral, merger, and ringdown of binary
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In this visualization a binary system containing two supermassive black holes and their accretion disks is initially viewed from above. After about 25 seconds, the camera tips close to the orbital plane to reveal the most dramatic distortions produced by their gravity. The different colors of the
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detector. As observed from Earth, a pair of black holes with estimated masses around 36 and 29 times that of the Sun spun into each other and merged to form an approximately 62-solar-mass black hole on 14 September 2015, at 09:50 UTC. Three solar masses were converted to gravitational
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can be used for the inspiral. These approximate the general-relativity field equations adding extra terms to equations in
Newtonian gravity. Orders used in these calculations may be termed 2PN (second-order post-Newtonian) 2.5PN or 3PN (third-order post-Newtonian). Effective-one-body (EOB)
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A number of solutions to the final-parsec problem have been proposed. Most involve mechanisms to bring additional matter, either stars or gas, close enough to the binary pair to extract energy from the binary and cause it to shrink. If enough stars pass close by to the orbiting pair, their
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For many years, proving the existence of binary black holes was made difficult because of the nature of black holes themselves and the limited means of detection available. However, in the event that a pair of black holes were to merge, an immense amount of energy should be given off as
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of each other. However, this process also ejects matter from the orbital path, and as the orbits shrink, the volume of space the black holes pass through reduces, until there is so little matter remaining that it could not cause a merger within the age of the universe.
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Graham, Matthew J.; Djorgovski, S. G.; Stern, Daniel; Glikman, Eilat; Drake, Andrew J.; Mahabal, Ashish A.; Donalek, Ciro; Larson, Steve; Christensen, Eric (7 January 2015). "A possible close supermassive black-hole binary in a quasar with optical periodicity".
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The gravitational waveform produced is important for observation prediction and confirmation. When inspiralling reaches the strong zone of the gravitational field, the waves scatter within the zone producing what is called the post-Newtonian tail (PN tail).
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For collisionless cold DM, the friction deposits so much energy that the spike is disrupted and cannot bridge the final parsec, while for self-interacting DM, the isothermal core of the halo can act as a reservoir for the energy liberated from the SMBH
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One mechanism that is known to work, although infrequently, is a third supermassive black hole from a second galactic collision. With three black holes in close proximity, the orbits are chaotic and allow three additional energy loss mechanisms:
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of gravitational wave flux. A technique to establish the radiation is the Cauchy-characteristic extraction technique CCE, which gives a close estimate of the flux at infinity, without having to calculate at larger and larger finite distances.
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Results from the calculations can include the binding energy. In a stable orbit the binding energy is a local minimum relative to parameter perturbation. At the innermost stable circular orbit the local minimum becomes an inflection point.
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from the other black hole. At this point in time the event horizon has a very narrow X-shape at the meeting point. The protrusions are drawn out into a thin thread. The meeting point expands to a roughly cylindrical connection called a
2154:
Capano, Collin D.; Cabero, Miriam; Westerweck, Julian; Abedi, Jahed; Kastha, Shilpa; Nitz, Alexander H.; Wang, Yi-Fan; Nielsen, Alex B.; Krishnan, Badri (28 November 2023). "Multimode
Quasinormal Spectrum from a Perturbed Black Hole".
34:
37:
33:
32:
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Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; et al. (The
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Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.; Allen, B.; Allen, G. S.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; et al.
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1202:
Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; et al.
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approximation solves the dynamics of the binary black-hole system by transforming the equations to those of a single object. This is especially useful where mass ratios are large, such as a stellar-mass black hole
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36:
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Komossa, S.; Burwitz, V.; Hasinger, G.; Predehl, P.; Kaastra, J. S.; Ikebe, Y. (2003-01-01). "Discovery of a Binary Active
Galactic Nucleus in the Ultraluminous Infrared Galaxy NGC 6240 Using Chandra".
170:
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We found that in most cases two of the three BHs merge through gravitational wave (GW) radiation in the timescale much shorter than the Hubble time, before ejecting one BH through a slingshot.
46:
as seen by a nearby observer, during its final inspiral, merge, and ringdown. The star field behind the black holes is being heavily distorted and appears to rotate and move, due to extreme
311:
As the black holesâ orbit shrinks, the speed increases, and gravitational wave emission increases. When the black holes are close the gravitational waves cause the orbit to shrink rapidly.
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produces a gravitation wave with the horizon frequency. In contrast, the
Schwarzschild black-hole ringdown looks like the scattered wave from the late inspiral, but with no direct wave.
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An unexpected result can occur with binary black holes that merge, in that the gravitational waves carry momentum, and the merging black-hole pair accelerates, seemingly violating
1103:
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Ori, Amos; Thorne, Kip S. (28 November 2000). "Transition from inspiral to plunge for a compact body in a circular equatorial orbit around a massive, spinning black hole".
1139:
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D'Orazio, Daniel J.; Haiman, ZoltĂĄn; Schiminovich, David (17 September 2015). "Relativistic boost as the cause of periodicity in a massive black-hole binary candidate".
1504:; Gopakumar, A.; Lehto, H. J.; Hyvönen, T.; Rampadarath, H.; Saunders, R.; Basta, M.; Hudec, R. (2010-02-01). "Measuring the Spin of the Primary Black Hole in OJ287".
2277:
Abbott, Benjamin P.; et al. (LIGO Scientific
Collaboration and Virgo Collaboration) (11 February 2016). "Properties of the binary black hole merger GW150914".
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PietilÀ, Harri; HeinÀmÀki, Pekka; Mikkola, Seppo; Valtonen, Mauri J. (1995). "Anisotropic gravitational radiation in the problems of three and four black holes".
209:
of the mobile SMBH in the galaxy J0437+2456 indicate that it is a promising candidate for hosting either a recoiling or binary SMBH, or an ongoing galaxy merger.
251:
Gravitational waves can cause significant loss of orbital energy, but not until the separation shrinks to a much smaller value, roughly 0.01â0.001 parsec.
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topology (ring-shaped). Some researchers suggested that it would be possible if, for example, several black holes in the same nearly circular orbit coalesce.
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When two galaxies collide, the supermassive black holes at their centers are very unlikely to hit head-on and would most likely shoot past each other on
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away. In its final 20 ms of spiraling inward and merging, GW150914 released around 3 solar masses as gravitational energy, peaking at a rate of 3.6
3322:
3422:
925:; Choi, Dae-Il; Koppitz, Michael; van Meter, James (2006). "Gravitational-Wave Extraction from an Inspiraling Configuration of Merging Black Holes".
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from Earth, between 600 million and 1.8 billion years ago. The observed signal is consistent with the predictions of numerical relativity.
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125:(detected September 2015, announced February 2016), a distinctive gravitational wave signature of two merging stellar-mass black holes of around 30
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The black holes orbit through a substantially larger volume of the galaxy, interacting with (and losing energy to) a much greater amount of matter.
1378:
Zhou, Hongyan; Wang, Tinggui; Zhang, Xueguang; Dong, Xiaobo; Li, Cheng (2004-03-20). "Obscured Binary Quasar Cores in SDSS J104807.74+005543.5?".
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This is followed by a plunging orbit, in which the two black holes meet, followed by the merger. Gravitational wave emission peaks at this time.
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axis of the initial orbit. It is calculated by integrating the product of the multipolar metric waveform with the news function complement over
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Campanelli, M.; Lousto, C. O.; Marronetti, P.; Zlochower, Y. (2006). "Accurate
Evolutions of Orbiting Black-Hole Binaries without Excision".
371:(200 solar masses per second), which is 50 times the total output power of all the stars in the observable universe. The merger took place
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Nonetheless, supermassive black holes appear to have merged, and what appears to be a pair in this intermediate range has been observed in
2018:
Iwasawa, Masaki; Funato, Yoko; Makino, Junichiro (2006). "Evolution of
Massive Blackhole Triples I â Equal-mass binaryâsingle systems".
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Lousto, Carlos; Zlochower, Yosef (2011). "Hangup Kicks: Still Larger
Recoils by Partial SpinâOrbit Alignment of Black-Hole Binaries".
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Description of the entire evolution, including merger, requires solving the full equations of general relativity. This can be done in
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number of points such that the numerical problem is tractable in a reasonable time, special coordinate systems can be used, such as
186:. Some likely candidates for binary black holes are galaxies with double cores still far apart. An example active double nucleus is
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Immediately following the merger, the now single black hole will "ring". This ringing is damped in the next stage, called the
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Smarr, Larry; ÄadeĆŸ, Andrej; DeWitt, Bryce; Eppley, Kenneth (1976). "Collision of two black holes: Theoretical framework".
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342:, by the emission of gravitational waves. The ringdown phase starts when the black holes approach each other within the
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198:. Other galactic nuclei have periodic emissions suggesting large objects orbiting a central black hole, for example, in
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Cohen, Michael I.; Kaplan, Jeffrey D.; Scheel, Mark A. (2012). "Toroidal horizons in binary black hole inspirals".
1961:"Interactions between multiple supermassive black holes in galactic nuclei: a solution to the final parsec problem"
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190:. Much closer black-hole binaries are likely in single-core galaxies with double emission lines. Examples include
3996:
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3412:
3160:
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Nichols, David A.; Chen, Yanbei (2012). "Hybrid method for understanding black-hole mergers: Inspiralling case".
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Pesce, D. W.; Seth, A. C.; Greene, J. E.; Braatz, J. A.; Condon, J. J.; Kent, B. R.; KrajnoviÄ, D. (March 2021).
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The existence of stellar-mass binary black holes (and gravitational waves themselves) was finally confirmed when
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in close orbit around each other. Like black holes themselves, binary black holes are often divided into binary
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This slows the black holes enough that they form a bound binary system, and further dynamical friction steals
191:
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87:
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232:, which transfers kinetic energy from the black holes to nearby matter. As a black hole passes a star, the
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put together. Supermassive binary black hole candidates have been found, but not yet categorically proven.
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Some simplified algebraic models can be used for the case where the black holes are far apart, during the
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1644:
1588:
1523:
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1397:
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1230:
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944:
866:
792:
574:, is the mass as measured at infinite distance and includes all the gravitational radiation emitted:
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gravitational ejection can bring the two black holes together in an astronomically plausible time.
142:
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2000:
1972:
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1892:"Self-Interacting Dark Matter Solves the Final Parsec Problem of Supermassive Black Hole Mergers"
1823:
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1016:
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229:
111:
107:
99:
75:
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3300:
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2801:
2707:
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2641:
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2516:
2473:
2408:
2373:) (2016-10-21). "Improved Analysis of GW150914 Using a Fully Spin-Precessing Waveform Model".
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1933:
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A milli-parsec supermassive black hole binary candidate in the galaxy SDSS J120136.02+300305.5
1044:
968:
960:
890:
882:
816:
808:
206:
141: – more than the combined power of all light radiated by all the stars in the
4001:
1873:"Don't Be So Cold â Self-Interacting Dark Matter as a Solution to the 'Final Parsec Problem'"
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83:
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Hahn, Susan G.; Lindquist, Richard W. (1964). "The two-body problem in geometrodynamics".
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PietilÀ, Harri; HeinÀmÀki, Pekka; Mikkola, Seppo; Valtonen, Mauri J. (10 January 1996).
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1986:
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is required to avoid the same problem of it all being ejected before the merger occurs.
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2340:"This collision was 50 times more powerful than all the stars in the universe combined"
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922:
456:
240:
1535:
1211:) (2016-02-11). "Observation of Gravitational Waves from a Binary Black Hole Merger".
1005:"Search for gravitational waves from binary black hole inspiral, merger, and ringdown"
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2004:
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183:
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at null infinity varied by solid angle. The
ArnowittâDeserâMisner (ADM) energy, or
285:, allowing energy loss by gravitational radiation at the point of closest approach.
255:
213:
2797:
2766:; Zlochower, Yosef; Merritt, David (7 June 2007). "Maximum Gravitational Recoil".
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accretion disks make it easier to track where light from each black hole turns up.
17:
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Damour, Thibault; Nagar, Alessandro; Pollney, Denis; Reisswig, Christian (2012).
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2075:"Introduction to LIGO & Gravitational Waves: Inspiral Gravitational Waves"
475:
382:
318:(ISCO) is the innermost complete orbit before the transition from inspiral to
288:
Two of the black holes can transfer energy to the third, possibly ejecting it.
228:, unless some mechanism brings them together. The most important mechanism is
216:
appears to have a binary black hole with an orbital period of 1900 days.
130:
126:
71:
51:
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is distorted, and the spectrum of frequencies it produces can be calculated.
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1995:
1960:
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2653:
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1937:
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1104:"Einstein was right: Scientists detect gravitational waves in breakthrough"
972:
894:
820:
656:{\displaystyle M_{\text{ADM}}=M_{\text{B}}(U)+\int _{-\infty }^{U}F(V)\,dV}
363:
radiation in the final fraction of a second, with a peak power 3.6Ă10
3916:
3875:
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2032:
1802:
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1295:"NASA Visualization Probes the Doubly Warped World of Binary Black Holes"
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571:
355:
304:
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122:
103:
43:
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1890:
Alonso-Ălvarez, Gonzalo; Cline, James M.; Dewar, Caitlyn (9 July 2024).
1725:
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The final mass of the resultant black hole depends on the definition of
153:
Stellar-mass binary black holes have been demonstrated to exist, by the
3956:
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2921:
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2105:
1819:
939:
861:
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Pretorius, Frans (2005). "Evolution of Binary Black-Hole Spacetimes".
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is also lost in the gravitational radiation. This is primarily in the
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3668:
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3257:
701:
368:
244:
27:
System consisting of two black holes in close orbit around each other
2945:"A Potential Recoiling Supermassive Black Hole CXO J101527.2+625911"
2253:"Gravitational waves detected 100 years after Einstein's prediction"
1959:; Haiman, ZoltĂĄn; Ostriker, Jeremiah P.; Stone, Nicholas C. (2018).
1071:"Observation Of Gravitational Waves From A Binary Black Hole Merger"
182:
Supermassive black-hole (SMBH) binaries are believed to form during
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1977:
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itself is distorted and dragged around by the rotating black holes.
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2618:
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1518:
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1171:
Liu, Fukun; Komossa, Stefanie; Schartel, Norbert (22 April 2014).
1021:
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The first observation of stellar-mass binary black holes merging,
258:. The question of how this happens is the "final-parsec problem".
199:
2735:
Anisotropic Gravitational Radiation In The Merger Of Black Holes
700:
Simulations as of 2011 had not produced any event horizons with
359:
158:
138:
118:
3081:
3077:
755:
364:
1567:"A Restless Supermassive Black Hole in the Galaxy J0437+2456"
685:
One of the problems to solve is the shape or topology of the
1173:"Unique Pair of Hidden Black Holes Discovered yy XMM-Newton"
302:
The first stage of the life of a binary black hole is the
2211:
Castelvecchi, Davide; Witze, Witze (February 11, 2016).
236:
accelerates the star while decelerating the black hole.
2602:"Energy Versus Angular Momentum in Black Hole Binaries"
1140:"Found! Gravitational Waves, or a Wrinkle in Spacetime"
842:
840:
838:
4050:
580:
554:) being the gravitational wave flux at retarded time
490:
484:
is calculated from the BondiâSach mass-loss formula,
916:
914:
912:
42:
Computer simulation of the black hole binary system
3894:
3746:
3708:
3687:
3626:
3585:
3534:
3400:
3293:
3203:
3128:
266:is also being considered, although it appears that
243:from the pair until they are orbiting within a few
655:
538:
462:The radiation reaction force can be calculated by
2206:
2204:
1965:Monthly Notices of the Royal Astronomical Society
1386:(1). The American Astronomical Society: L33âL36.
1325:(1). The American Astronomical Society: L15âL19.
1760:"More Evidence for Coming Black Hole Collision"
768:
766:
764:
413:, but can also be used for equal-mass systems.
2534:
2532:
2530:
2213:"Einstein's gravitational waves found at last"
3093:
1796:(1). American Institute of Physics: 201â210.
8:
2667:
2665:
2663:
455:In the ringdown phase of a Kerr black hole,
2891:Celestial Mechanics and Dynamical Astronomy
756:SXS (Simulating eXtreme Spacetimes) project
3659:Magnetospheric eternally collapsing object
3100:
3086:
3078:
539:{\displaystyle {\frac {dM_{B}}{dU}}=-f(U)}
3561:
3060:
3042:
2980:
2962:
2911:
2840:
2779:
2746:
2685:
2635:
2617:
2552:
2386:
2290:
2168:
2104:
2031:
1994:
1976:
1927:
1909:
1850:. Princeton: Princeton University Press.
1847:Dynamics and Evolution of Galactic Nuclei
1801:
1707:
1638:
1600:
1582:
1517:
1460:
1391:
1330:
1224:
1030:
1020:
938:
860:
786:
646:
628:
620:
598:
585:
579:
501:
491:
489:
157:of a black-hole merger event GW150914 by
78:, formed either as remnants of high-mass
1197:
1195:
1193:
1076:. LIGO. 11 February 2016. Archived from
163:
29:
4057:
747:
411:merging with a galactic-core black hole
398:stage, and also to solve for the final
129:each, occurring about 1.3 billion
2426:
2086:
2084:
1272:
3027:"Massive Black Hole Binary Evolution"
1439:Gerke, Brian F.; Newman, Jeffrey A.;
7:
4035:
3010:Binary Black Holes Orbit and Collide
2739:Relativistic Astrophysics Conference
2259:. NSF â National Science Foundation
714:Pulsar kick § Black hole kicks
2338:Kramer, Sarah (11 February 2016).
624:
25:
1449:The Astrophysical Journal Letters
4132:
4120:
4108:
4096:
4084:
4072:
4060:
4034:
4025:
4024:
3323:TolmanâOppenheimerâVolkoff limit
3194:
2943:Kim, D.-C.; et al. (2017).
2077:. LIGO Scientific Collaboration.
1102:Harwood, W. (11 February 2016).
736:List of most massive black holes
70:, is a system consisting of two
3440:Innermost stable circular orbit
3025:; MilosavljeviÄ, MiloĆĄ (2005).
2137:"For whom the black hole rings"
1871:Lamb, William (8 August 2024).
316:innermost stable circular orbit
86:and mutual capture; and binary
3866:Timeline of black hole physics
2859:10.1103/PhysRevLett.107.231102
2637:10.1103/PhysRevLett.108.131101
2309:10.1103/PhysRevLett.116.241102
2187:10.1103/PhysRevLett.131.221402
1929:10.1103/PhysRevLett.133.021401
1500:Valtonen, M. J.; Mikkola, S.;
1243:10.1103/PhysRevLett.116.061102
643:
637:
610:
604:
533:
527:
1:
3634:Nonsingular black hole models
2798:10.1103/PhysRevLett.98.231102
2433:: CS1 maint: date and year (
2367:LIGO Scientific Collaboration
1279:: CS1 maint: date and year (
1205:LIGO Scientific Collaboration
997:LIGO Scientific Collaboration
957:10.1103/PhysRevLett.96.111102
879:10.1103/PhysRevLett.96.111101
805:10.1103/PhysRevLett.95.121101
416:For the ringdown, black-hole
406:Post-Newtonian approximations
281:The orbits can become highly
112:directly detecting such waves
106:that can be calculated using
90:, believed to be a result of
3031:Living Reviews in Relativity
2470:10.1016/0003-4916(64)90223-4
689:during a black-hole merger.
268:self-interacting dark matter
3856:Rossi X-ray Timing Explorer
3821:Hypercompact stellar system
3811:Gamma-ray burst progenitors
1536:10.1088/0004-637X/709/2/725
434:BoyerâLindquist coordinates
4176:
3542:Black hole complementarity
3509:Bousso's holographic bound
3494:Quasi-periodic oscillation
3192:
3186:MalamentâHogarth spacetime
2704:10.1103/PhysRevD.85.024031
2571:10.1103/PhysRevD.85.044035
2123:10.1103/PhysRevD.62.124022
1790:AIP Conference Proceedings
1783:"The Final Parsec Problem"
1041:10.1103/PhysRevD.83.122005
711:
472:mass in general relativity
4020:
3413:Gravitational singularity
3115:
2405:10.1103/PhysRevX.6.041014
2225:10.1038/nature.2016.19361
1506:The Astrophysical Journal
1380:The Astrophysical Journal
1319:The Astrophysical Journal
436:or fish-eye coordinates.
314:The last stable orbit or
196:EGSD2 J142033.66 525917.5
3997:PSO J030947.49+271757.31
3922:SDSS J150243.09+111557.3
3455:BlandfordâZnajek process
2982:10.3847/1538-4357/aa6030
2513:10.1103/PhysRevD.14.2443
1602:10.3847/1538-4357/abde3d
1145:National Geographic News
708:Black-hole merger recoil
192:SDSS J104807.74+005543.5
88:supermassive black holes
3253:Active galactic nucleus
2829:Physical Review Letters
2768:Physical Review Letters
2606:Physical Review Letters
2279:Physical Review Letters
2157:Physical Review Letters
1897:Physical Review Letters
1213:Physical Review Letters
927:Physical Review Letters
849:Physical Review Letters
775:Physical Review Letters
420:can be used. The final
358:, was performed by the
234:gravitational slingshot
226:hyperbolic trajectories
3881:Tidal disruption event
3851:Supermassive dark star
3769:Black holes in fiction
3754:Outline of black holes
3387:Supermassive dark star
3306:Gravitational collapse
1777:MilosavljeviÄ, MiloĆĄ;
657:
540:
179:
55:
3759:Black Hole Initiative
3572:Holographic principle
2950:Astrophysical Journal
2762:Campanelli, Manuela;
1996:10.1093/mnras/stx2524
1758:(16 September 2015).
1571:Astrophysical Journal
1297:. NASA. 15 April 2021
658:
541:
440:black holes in 2005.
220:Final-parsec problem
176:
48:gravitational lensing
41:
3562:Final parsec problem
3521:Schwarzschild radius
1138:(11 February 2016).
578:
488:
429:numerical relativity
205:Measurements of the
3861:Superluminal motion
3836:Population III star
3806:Gravitational waves
3764:Black hole starship
3547:Information paradox
3062:10.12942/lrr-2005-8
3053:2005LRR.....8....8M
2973:2017ApJ...840...71K
2904:1995CeMDA..62..377P
2851:2011PhRvL.107w1102L
2790:2007PhRvL..98w1102C
2696:2012PhRvD..85b4031C
2628:2012PhRvL.108m1101D
2563:2012PhRvD..85d4035N
2505:1976PhRvD..14.2443S
2462:1964AnPhy..29..304H
2397:2016PhRvX...6d1014A
2371:Virgo Collaboration
2301:2016PhRvL.116x1102A
2179:2023PhRvL.131v1402C
2115:2000PhRvD..62l4022O
2042:2006ApJ...651.1059I
1987:2018MNRAS.473.3410R
1920:2024PhRvL.133b1401A
1812:2003AIPC..686..201M
1726:10.1038/nature15262
1718:2015Natur.525..351D
1657:10.1038/nature14143
1649:2015Natur.518...74G
1593:2021ApJ...909..141P
1528:2010ApJ...709..725V
1471:2007ApJ...660L..23G
1402:2004ApJ...604L..33Z
1341:2003ApJ...582L..15K
1235:2016PhRvL.116f1102A
1209:Virgo Collaboration
1152:on 12 February 2016
1116:on 12 February 2016
1083:on 16 February 2016
1032:2011PhRvD..83l2005A
1001:Virgo Collaboration
949:2006PhRvL..96k1102B
871:2006PhRvL..96k1101C
797:2005PhRvL..95l1101P
633:
418:perturbation theory
143:observable universe
102:, with distinctive
100:gravitational waves
76:stellar black holes
3695:Optical black hole
3608:ReissnerâNordström
3567:Firewall (physics)
3472:Gravitational lens
2922:10.1007/BF00692287
1764:The New York Times
724:Newton's third law
653:
616:
536:
390:Dynamics modelling
230:dynamical friction
180:
108:general relativity
56:
18:Binary black holes
4048:
4047:
3841:Supermassive star
3831:Naked singularity
3826:Membrane paradigm
3552:Cosmic censorship
3526:Spaghettification
3514:Immirzi parameter
3467:Hawking radiation
3408:Astrophysical jet
3377:Supermassive star
3367:Binary black hole
3301:Stellar evolution
3243:Intermediate-mass
2674:Physical Review D
2541:Physical Review D
2499:(10): 2443â2452.
2493:Physical Review D
2450:Annals of Physics
2375:Physical Review X
2093:Physical Review D
1857:978-0-691-12101-7
1820:10.1063/1.1629432
1702:(7569): 351â353.
1009:Physical Review D
601:
588:
516:
207:peculiar velocity
174:
84:dynamic processes
68:black hole binary
60:binary black hole
39:
16:(Redirected from
4167:
4137:
4136:
4125:
4124:
4123:
4113:
4112:
4111:
4101:
4100:
4099:
4089:
4088:
4077:
4076:
4075:
4065:
4064:
4056:
4038:
4037:
4028:
4027:
3700:Sonic black hole
3649:Dark-energy star
3504:Bekenstein bound
3489:Mâsigma relation
3418:Ring singularity
3198:
3102:
3095:
3088:
3079:
3074:
3064:
3046:
3044:astro-ph/0410364
3018:
2995:
2994:
2984:
2966:
2940:
2934:
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2915:
2885:
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2240:
2239:
2208:
2199:
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2151:
2145:
2144:
2133:
2127:
2126:
2108:
2088:
2079:
2078:
2071:
2065:
2064:
2035:
2033:astro-ph/0511391
2026:(2): 1059â1067.
2015:
2009:
2008:
1998:
1980:
1971:(3): 3410â3433.
1952:
1946:
1945:
1931:
1913:
1887:
1881:
1880:
1868:
1862:
1861:
1838:
1832:
1831:
1805:
1803:astro-ph/0212270
1787:
1781:(October 2003).
1774:
1768:
1767:
1752:
1746:
1745:
1711:
1691:
1685:
1684:
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1555:
1521:
1497:
1491:
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1464:
1462:astro-ph/0608380
1436:
1430:
1429:
1395:
1393:astro-ph/0411167
1375:
1369:
1368:
1334:
1332:astro-ph/0212099
1313:
1307:
1306:
1304:
1302:
1291:
1285:
1284:
1278:
1270:
1228:
1199:
1188:
1187:
1185:
1183:
1168:
1162:
1161:
1159:
1157:
1148:. Archived from
1132:
1126:
1125:
1123:
1121:
1112:. Archived from
1099:
1093:
1092:
1090:
1088:
1082:
1075:
1067:
1061:
1060:
1034:
1024:
1003:) (2011-06-06).
991:
985:
984:
942:
921:Baker, John G.;
918:
907:
906:
864:
844:
833:
832:
790:
770:
759:
752:
718:Rogue black hole
667:Angular momentum
662:
660:
659:
654:
632:
627:
603:
602:
599:
590:
589:
586:
564:surface integral
545:
543:
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517:
515:
507:
506:
505:
492:
464:Padé resummation
385:
380:
379:
175:
136:
92:galactic mergers
40:
21:
4175:
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4145:
4144:
4143:
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4119:
4109:
4107:
4097:
4095:
4083:
4073:
4071:
4059:
4051:
4049:
4044:
4016:
3992:ULAS J1342+0928
3952:SDSS J0849+1114
3937:Phoenix Cluster
3890:
3742:
3704:
3683:
3622:
3581:
3577:No-hair theorem
3530:
3484:Bondi accretion
3450:Penrose process
3396:
3362:Gamma-ray burst
3289:
3199:
3190:
3176:Direct collapse
3124:
3111:
3106:
3021:
3007:
3004:
2999:
2998:
2942:
2941:
2937:
2887:
2886:
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2826:
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2012:
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1870:
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1835:
1785:
1776:
1775:
1771:
1756:Overbye, Dennis
1754:
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923:Centrella, Joan
920:
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422:Kerr black hole
392:
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164:
155:first detection
151:
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30:
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5:
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4012:Swift J1644+57
4009:
4004:
3999:
3994:
3989:
3984:
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3974:
3969:
3964:
3962:MS 0735.6+7421
3959:
3954:
3949:
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3939:
3934:
3929:
3927:Sagittarius A*
3924:
3919:
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3506:
3501:
3499:Thermodynamics
3496:
3491:
3486:
3481:
3480:
3479:
3469:
3464:
3462:Accretion disk
3459:
3458:
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3178:
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3153:
3148:
3143:
3138:
3136:BTZ black hole
3132:
3130:
3126:
3125:
3123:
3122:
3116:
3113:
3112:
3107:
3105:
3104:
3097:
3090:
3082:
3076:
3075:
3023:Merritt, David
3019:
3003:
3002:External links
3000:
2997:
2996:
2935:
2913:10.1.1.51.2616
2898:(4): 377â394.
2880:
2835:(23): 231102.
2819:
2774:(23): 231102.
2764:Lousto, Carlos
2754:
2748:10.1.1.51.2616
2725:
2659:
2612:(13): 131101.
2592:
2526:
2483:
2456:(2): 304â331.
2440:
2356:
2330:
2285:(24): 241102.
2269:
2244:
2200:
2163:(22): 221402.
2146:
2141:www.aei.mpg.de
2128:
2099:(12): 124022.
2080:
2066:
2050:10.1086/507473
2010:
1957:Perna, Rosalba
1947:
1882:
1863:
1856:
1842:Merritt, David
1833:
1779:Merritt, David
1769:
1747:
1686:
1633:(7537): 74â6.
1616:
1577:(2): 141â153.
1557:
1512:(2): 725â732.
1492:
1479:10.1086/517968
1455:(1): L23âL26.
1441:Lotz, Jennifer
1431:
1410:10.1086/383310
1370:
1349:10.1086/346145
1308:
1286:
1189:
1163:
1127:
1094:
1062:
1015:(12): 122005.
986:
933:(11): 111102.
908:
855:(11): 111101.
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584:
535:
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481:
457:frame-dragging
391:
388:
351:
348:
335:
332:
327:
324:
299:
296:
294:
291:
290:
289:
286:
279:
241:orbital energy
221:
218:
184:galaxy mergers
150:
147:
82:systems or by
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
4172:
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4019:
4013:
4010:
4008:
4005:
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4000:
3998:
3995:
3993:
3990:
3988:
3987:Markarian 501
3985:
3983:
3980:
3978:
3975:
3973:
3970:
3968:
3965:
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3925:
3923:
3920:
3918:
3915:
3913:
3912:XTE J1118+480
3910:
3908:
3907:XTE J1650-500
3905:
3903:
3900:
3899:
3897:
3893:
3887:
3884:
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3625:
3619:
3616:
3614:
3611:
3609:
3606:
3604:
3601:
3598:
3594:
3593:Schwarzschild
3591:
3590:
3588:
3584:
3578:
3575:
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3460:
3456:
3453:
3451:
3448:
3447:
3446:
3443:
3441:
3438:
3436:
3435:Photon sphere
3433:
3431:
3430:Event horizon
3428:
3424:
3421:
3419:
3416:
3415:
3414:
3411:
3409:
3406:
3405:
3403:
3399:
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3356:
3355:Related links
3353:
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3338:
3334:
3333:Related links
3331:
3330:
3329:
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3317:
3316:Related links
3314:
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3141:Schwarzschild
3139:
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3127:
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3110:
3103:
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2823:
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2815:
2811:
2807:
2803:
2799:
2795:
2791:
2787:
2782:
2781:gr-qc/0702133
2777:
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2769:
2765:
2758:
2755:
2749:
2744:
2740:
2736:
2729:
2726:
2721:
2717:
2713:
2709:
2705:
2701:
2697:
2693:
2688:
2683:
2680:(2): 024031.
2679:
2675:
2668:
2666:
2664:
2660:
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2647:
2643:
2638:
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2547:(4): 044035.
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2381:(4): 041014.
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2166:
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2158:
2150:
2147:
2142:
2138:
2132:
2129:
2124:
2120:
2116:
2112:
2107:
2106:gr-qc/0003032
2102:
2098:
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2076:
2070:
2067:
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2059:
2055:
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2025:
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2014:
2011:
2006:
2002:
1997:
1992:
1988:
1984:
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1966:
1962:
1958:
1951:
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1232:
1227:
1222:
1219:(6): 061102.
1218:
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1210:
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1190:
1178:
1174:
1167:
1164:
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1002:
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990:
987:
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966:
962:
958:
954:
950:
946:
941:
940:gr-qc/0511103
936:
932:
928:
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917:
915:
913:
909:
904:
900:
896:
892:
888:
884:
880:
876:
872:
868:
863:
862:gr-qc/0511048
858:
854:
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843:
841:
839:
835:
830:
826:
822:
818:
814:
810:
806:
802:
798:
794:
789:
788:gr-qc/0507014
784:
780:
776:
769:
767:
765:
761:
757:
751:
748:
741:
737:
734:
733:
729:
727:
725:
719:
715:
707:
705:
703:
698:
696:
690:
688:
687:event horizon
680:
678:
676:
675:retarded time
672:
668:
664:
650:
647:
640:
634:
629:
621:
617:
613:
607:
595:
591:
582:
573:
569:
568:news function
565:
561:
557:
553:
549:
530:
524:
521:
518:
512:
509:
502:
498:
494:
480:
477:
473:
468:
465:
460:
458:
453:
449:
445:
441:
437:
435:
430:
425:
423:
419:
414:
412:
407:
403:
401:
397:
389:
387:
384:
370:
366:
361:
357:
349:
347:
345:
344:photon sphere
341:
333:
331:
325:
323:
321:
317:
312:
309:
307:
306:
297:
292:
287:
284:
280:
277:
276:
275:
271:
269:
265:
259:
257:
252:
249:
246:
242:
237:
235:
231:
227:
219:
217:
215:
210:
208:
203:
201:
197:
193:
189:
185:
162:
160:
156:
148:
146:
144:
140:
132:
128:
124:
120:
115:
113:
109:
105:
101:
95:
93:
89:
85:
81:
77:
73:
69:
65:
61:
53:
49:
45:
19:
4160:Binary stars
4127:Solar System
3942:PKS 1302-102
3816:Gravity well
3784:Compact star
3738:Microquasars
3723:Most massive
3627:Alternatives
3392:X-ray binary
3366:
3311:Neutron star
3248:Supermassive
3225:Hawking star
3166:Supermassive
3034:
3030:
3013:– via
3009:
2957:(2): 71â77.
2954:
2948:
2938:
2895:
2889:
2883:
2832:
2828:
2822:
2771:
2767:
2757:
2738:
2734:
2728:
2677:
2673:
2609:
2605:
2595:
2544:
2540:
2496:
2492:
2486:
2453:
2449:
2443:
2429:cite journal
2378:
2374:
2359:
2347:. Retrieved
2344:Tech Insider
2343:
2333:
2282:
2278:
2272:
2261:. Retrieved
2256:
2247:
2236:. Retrieved
2216:
2160:
2156:
2149:
2140:
2131:
2096:
2092:
2069:
2061:
2023:
2020:Astrophys. J
2019:
2013:
1968:
1964:
1955:Ryu, Taeho;
1950:
1941:
1904:(2) 021401.
1901:
1895:
1885:
1876:
1866:
1846:
1836:
1793:
1789:
1772:
1763:
1750:
1699:
1695:
1689:
1630:
1626:
1619:
1574:
1570:
1560:
1509:
1505:
1495:
1452:
1448:
1444:
1434:
1383:
1379:
1373:
1322:
1318:
1311:
1299:. Retrieved
1289:
1275:cite journal
1216:
1212:
1180:. Retrieved
1176:
1166:
1154:. Retrieved
1150:the original
1143:
1136:Drake, Nadia
1130:
1118:. Retrieved
1114:the original
1107:
1097:
1085:. Retrieved
1078:the original
1065:
1012:
1008:
989:
930:
926:
852:
848:
778:
774:
750:
721:
699:
694:
691:
684:
670:
665:
559:
555:
551:
547:
478:
469:
461:
454:
450:
446:
442:
438:
426:
415:
404:
399:
395:
393:
353:
339:
337:
329:
319:
313:
310:
303:
301:
272:
260:
256:PKS 1302-102
253:
250:
238:
223:
214:PKS 1302-102
211:
204:
181:
152:
127:solar masses
116:
96:
67:
63:
59:
57:
4155:Black holes
4115:Outer space
4103:Spaceflight
3932:Centaurus A
3886:Planet Nine
3789:Exotic star
3718:Black holes
3664:Planck star
3613:KerrâNewman
3328:White dwarf
3278:Radio-Quiet
3236:Microquasar
3109:Black holes
2349:12 February
2257:www.nsf.gov
2217:Nature News
1502:Merritt, D.
1182:23 December
1156:12 February
1120:12 February
1087:11 February
383:megaparsecs
350:Observation
264:Dark matter
212:The quasar
131:light-years
80:binary star
72:black holes
4149:Categories
3982:Q0906+6930
3972:Hercules A
3902:Cygnus X-1
3871:White hole
3846:Quasi-star
3799:Preon star
3794:Quark star
3779:Big Bounce
3639:Black star
3597:Derivation
3445:Ergosphere
3401:Properties
3382:Quasi-star
3372:Quark star
3283:Radio-Loud
3171:Primordial
3161:Kugelblitz
2964:1704.05549
2388:1606.01210
2292:1602.03840
2263:2016-02-11
2238:2016-02-11
2170:2105.05238
1978:1709.06501
1911:2401.14450
1877:Astrobites
1709:1509.04301
1640:1501.01375
1584:2101.07932
1226:1602.03837
742:References
712:See also:
476:Bondi mass
149:Occurrence
52:space-time
4079:Astronomy
4007:AT2018hyz
3654:Gravastar
3644:Dark star
3477:Microlens
3350:Hypernova
3345:Micronova
3340:Supernova
3294:Formation
3071:119367453
2991:119401892
2930:122956625
2908:CiteSeerX
2842:1108.2009
2743:CiteSeerX
2712:1550-7998
2687:1110.1668
2646:0031-9007
2619:1110.2938
2579:1550-7998
2554:1109.0081
2521:0556-2821
2478:0003-4916
2413:2160-3308
2325:217406416
2233:182916902
2005:119083047
1742:205245606
1665:0028-0836
1611:231648121
1552:119276181
1544:0004-637X
1519:0912.1209
1418:0004-637X
1357:0004-637X
1267:124959784
1251:0031-9007
1049:1550-7998
1022:1102.3781
965:0031-9007
887:0031-9007
813:0031-9007
754:Credits:
625:∞
622:−
618:∫
522:−
293:Lifecycle
283:eccentric
121:detected
104:waveforms
4030:Category
3917:A0620-00
3876:Wormhole
3774:Big Bang
3674:Fuzzball
3557:ER = EPR
3423:Theorems
3221:Electron
3216:Extremal
3146:Rotating
2875:15546595
2867:22182078
2814:29246347
2806:17677894
2720:37654897
2654:22540688
2587:30890236
2421:18217435
2369:and The
2317:27367378
2195:38101361
2058:14816623
1938:39073950
1844:(2013).
1828:12124842
1734:26381982
1673:25561176
1487:14320681
1447:= 0.7".
1426:14297940
1365:16697327
1301:16 April
1259:26918975
1109:CBS News
981:23409406
973:16605809
895:16605808
829:24225193
821:16197061
730:See also
702:toroidal
572:ADM mass
400:ringdown
396:inspiral
356:GW150914
340:ringdown
334:Ringdown
305:inspiral
298:Inspiral
188:NGC 6240
137:10
123:GW150914
44:GW150914
4139:Science
4067:Physics
4053:Portals
4040:Commons
4002:P172+18
3957:TON 618
3895:Notable
3747:Related
3733:Quasars
3728:Nearest
3688:Analogs
3618:Hayward
3586:Metrics
3231:Stellar
3156:Virtual
3151:Charged
3120:Outline
3049:Bibcode
3015:YouTube
2969:Bibcode
2900:Bibcode
2847:Bibcode
2786:Bibcode
2692:Bibcode
2624:Bibcode
2559:Bibcode
2501:Bibcode
2458:Bibcode
2393:Bibcode
2297:Bibcode
2175:Bibcode
2111:Bibcode
2038:Bibcode
1983:Bibcode
1943:orbits.
1916:Bibcode
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