In General > s.a. gravitational
phenomenology / astronomy; higher-dimensional
black holes; sources of
* History: The idea of the existence of black holes seemed reasonable only after the discovery of pulsars in 1968.
* Status: 2005, Dozens of compact objects with M > 3 Msun are known, and identified as black-hole candidates; Stellar ones, with masses up to about 20 Msun, are found as unseen companions in low-mass X-ray binaries, the rest have masses from a million to a billion Msun and are found in galactic nuclei; There is strong circumstantial evidence that many of them have event horizons.
* Parameters: The simplest black hole parameter to measure is the mass; We do not expect to find black holes with appreciable electric charge; A variety of methods are being tried to estimate their spin parameters, such as the polarization of X-rays emitted very close to the event horizon (in 1995 this was still not possible).
* Remark: The notion of event horizon is a global one; The local analogs are those of trapped surface, or isolated/dynamical horizon.
@ Texts. Reviews: Lasota SA(99)may; Rees in(03)ap/04; Cherepashchuk gq/05-conf [search]; van Putten 05; Bilić PoS(06)ap [especially X-ray binaries]; Müller PoS(06)ap/07 [evidence]; Romero a0805-ln; Czerny & Nikolajuk a0910-proc [masses]; Narayan & McClintock a1312-in [observational evidence]; Bailyn 14.
@ Astrophysics: Narayan NJP(05)ap; Romero & Vila 14; Merritt & Rezzolla ed-CQG(13)#24; Haardt et al ed-16.
@ Falling in: Tammelo & Kask GRG(97) [passage through horizon]; Krasnikov G&C(08)-a0804, Augousti et al EJP(12) [pedagogical].
@ Collisions, mergers: Berti et al PRD(10)-a1003 [ultrarelativistic, scattering thresholds and gravitational radiation]; Gerosa & Berti a1703 [and gravitational wave observations].
> Types of phenomena: see binaries; matter and radiation near black holes [including acceleration, jets, accretion disks]; gamma-ray astronomy.
Stages in Black Hole Evolution > s.a. black-hole
formation and radiation.
* Evaporation: After black-hole formation, in addition to possible growth by accretion of additional matter, the stages are (i) Balding, in which the black hole loses its hair and becomes stationary; (ii) Hawking radiation, in which the black hole shrinks; and (iii) Quantum gravity phase, about which we still don't know much.
* Hawking radiation: For small black holes, look for γ-rays over the background.
@ General references: Adams et al PLB(99) [effect of a cosmological constant on radiation]; Dalal & Griest PLB(00)ap [all eventually evaporate]; Ashtekar et al PRD(13)-a1306 [dynamics of horizon multipole moments and approach to the final state].
@ Hawking radiation: Stephens PLA(89); Rosu IJMPD(94)gq/96, NCB(93)gq/95, MPLA(93)gq/97, MPLA(98), G&C(01)gq/94.
Detection and Observation > s.a. analogs
[and mimickers]; binaries; black-hole
geometry [interior]; types
of black holes; supermassive
* Observation: A stationary, isolated black hole, with no matter around it and no objects in the background, cannot be seen; One with matter around it can be identified by the behavior of the matter, although because of the infinite gravitational redshift at the horizon, the horizon or the matter crossing it will never be seen from the outside (what one can see instead is a "frozen star"); One with objects behind it can be identified from its lensing effects.
* Candidates: 2008, There are many, in a range of masses from stellar ones to supermassive ones in galactic cores, but no definitive evidence that they really are black holes; Although some people say that it is possible to observe effects arising from the presence of a horizon, the most convincing type may be the detection of the specific frequencies predicted for quasinormal modes, for example in ringdowns after mergers; 2016, We now know a few with masses in the tens of solar masses, from gravitational-wave observations.
@ Appearance: Ames & Thorne ApJ(68); de Felice & Usseglio-Tomasset CQG(93) [orbiting]; Nemiroff AJP(93)jul-ap; Stuckey AJP(93)may [surrounding objects]; Marck CQG(96)gq/95; Zakharov et al gq/05-conf; Vachaspati et al PRD(07)-gq/06 [from quantum collapse]; Zhang IJMPD(11)-a1003-conf [frozen stars]; Müller & Boblest AJP(11)jan [observer on a circular orbit around a Schwarzschild black hole]; Müller & Frauendiener EJP(12)-a1206 [thin disk around a Schwarzschild black hole]; Cardoso et al PRD(14)-a1406 [light rings as evidence]; news wired(14)oct [the movie Interstellar]; > s.a. black-hole geometry [interior].
@ Determining black-hole spin: Mukhopadhyay et al IJMPD(12)-a1210; Pürrer et al PRD(16)-a1512 [from gravitational-wave observations].
@ Testing the Kerr hypothesis: Bambi MPLA(11)-a1109, PRD(12); Bambi PRD(12)-a1204 [black-hole spin and power of steady jets]; Bambi JCAP(12)-a1205; Bambi AR(13)-a1301 [with radio and X-ray data]; Li & Bambi JCAP(14) [Kerr spin parameter and black-hole shadow].
@ Shadows: Abdolrahimi et al PRD(15)-a1502 [local]; Amarilla & Eiroa a1512-proc [in alternative theories]; Younsi et al PRD(16)-a1607 [calculation method].
@ Related topics: Firouzjaee et al GRG(12)-a1010 [mass]; Fender et al MNRAS(13)-a1301 [how to search for the closest black holes]; Middleton ch(16)-a1507 [spin, theory and observation]; Lu et al MNRAS-a1702 [evidence for event horizons].
> And other theories of gravity: see astrophysical tests of general relativity; detection of gravitational waves; massive gravity.
Other Effects and Properties > s.a. astrophysics;
matter in kerr backgrounds
* Rotating black holes: According to a calculation by K Thorne, the maximum value of a allowed for a rotating (Kerr) black hole spun up by accreting matter is 0.998; This is a conservative bound, however, and more recent simulations suggest that the limit is at most 0.93.
* Retro-MACHOs: A black hole may act as a retro-lens which, if illuminated by a powerful light source, deflects light ray paths to large bending angles, allowing us to detect the black hole.
@ Quantum gravity effects: Flambaum gq/04 [particle and radiation phenomena]; Marolf GRG(10)-a1005-GRF [microphysics outside extreme or nearly extreme black holes]; Giddings PRD(14)-a1406 [possible observational windows]; Chen et al IJMPA(14)-a1410 [rev]; Giddings a1602 [gravitational-wave tests]; > s.a. quantum black holes
@ General references: Ruffini ap/98-proc [electromagnetic particle production]; Dimopoulous & Landsberg PRL(01) + pn(01)sep [in the lab?]; Jacobson & Sotiriou a1006-FQXi [on whether it is possible to destroy the event horizon]; Berti BJP(13)-a1302-TX [fundamental physics and strong-field gravity].
@ As retro-MACHOs: Holz & Wheeler ApJ(02)ap [Schwarzschild]; De Paolis et al A&A(04)ap, Zakharov et al ap/04/A&A [Kerr].
@ Rotating black holes: Poisson PRD(09)-a0907 [tidal interactions]; Yang et al PRL(15)-a1402 [rapidly-spinning black holes, turbulent gravitational behavior]; Poisson PRD(15)-a1411 [tidal deformations]; Herdeiro & Radu IJMPD(15)-a1505-GRF [bound on rotation speed].
@ Frame dragging: Wex ap/99-conf; Konno et al PRD(08)-a0807 [in Chern-Simons-modified gravity]; Herdeiro et al PRD(09)-a0907 [back-reaction]; Karas et al JPCS(12)-a1202 [on magnetic fields].
@ Magnetosphere: Ghosh MNRAS(00)ap/99; Nathanail & Contopoulos ApJ(14)-a1404; Lupsasca et al JHEP(14)-a1406 [force-free electrodynamics]; > s.a. kerr.
@ Accelerating black holes: Podolský et al PRD(03)gq [radiation, in Anti-de Sitter]; > s.a. c-metric.
@ Nearly-extremal black holes: Jacobson PRD(98)ht/97 [decay]; Garfinkle CQG(11) [infalling observers].
@ Related topics: Hsu PLB(02) [parity]; Gott & Freedman ap/03/PRD [life preserver]; Bekenstein in(03)gq [preparing a desired black hole]; news pw(08)apr [blazars]; Crane & Westmoreland a0908 [black-hole-powered spaceships]; Dokuchaev & Eroshenko AHEP(14)-a1403 [black-hole atoms]; > s.a. black-hole geometry [interior]; black-hole uniqueness; brane-world gravity; vacuum [vacuum decay nucleation sites]; Porto FdP(16)-a1606 [and the nature of spacetime].
> And cosmology: see multiverse; variation of constants.
> Related topics: see fine-structure constant; Gyromagnetic Ratio; Mass Inflation; particle models; quantum cloning; wormholes.
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