Black Hole Analogs and Mimickers  

In General > s.a. lorentzian geometry [analog gravity]; modified general relativity; sound [differential geometric approach].
* Remark: Black holes are like spacetime rivers, in that their geometry can be viewed as if space were a moving medium rushing towards their singularities; Horizons are formed where the flow speed exceeds the speed of light such that nothing can escape anymore.
* Idea: Systems in which perturbations of a medium (e.g., acoustic or electromagnetic waves) cannot leave a region of space, for reasons other than spacetime curvature due to gravity; Can often be modeled by an effective curved geometry, and are useful for studying features of black holes, including their possible realization in the lab.
@ General references: Novello et al CQG(03)gq/02 [flowing dielectrics]; Jacobson & Koike cm/02-in [thin film of 3He-A]; Novello et al ed-02.
@ Radiation: Srinivasan & Padmanabhan gq/98; Pauri & Vallisneri FP(99)gq; Sakagami & Ohashi PTP(02)gq/01 [in the lab]; Schützhold & Unruh PRL(05)qp/04 [electromagnetic waveguide]; Barceló et al CQG(06)gq, PRL(06)gq [quasi-particle creation]; Kim & Shin a0706 [anomaly cancelation method].
@ Radiation, acoustic black holes: Unruh PRL(81), PRD(95)gq/94 [and high-energy dispersion relations]; Visser CQG(98)gq/97; Giovanazzi PRL(05); Balbinot et al RNC(05)gq/06.
@ Black-hole-mimicking spacetimes / doubles: Lemos & Zaslavskii a0806; > s.a. Ergoregion [instabilities].

For Acoustic Waves
* Idea: Fluid dynamic analogs of general relativistic black holes, where the behaviour of sound waves in a moving fluid acts as an analog for scalar fields in a gravitational background; The analog of the event horizon occurs where the bulk speed of the fluid coincides with the propagation speed of acoustic waves in the fluid.
* Motivation: Acoustic horizons possess many of the properties normally associated with the event horizons of general relativity, including Hawking radiation, and have received much attention because it would seem to be much easier to experimentally create an acoustic horizon than to create an event horizon; However, so far (2005) the Hawking temperature seems to be too low for radiation to be detected, TH (10–9/rH(m)) K, because the thermal noise would be too high.
@ Reviews, intros: Visser gq/99-in; Cardoso phy/05-in; Jacobson & Parentani SA(05)dec.
@ General references: Jacobson & Volovik PRD(98)cm, JETPL(98)gq [3He]; Basak & Majumdar CQG(03)gq/02 [rotating]; Parentani IJMPA(02)gq-in; Visser & Weinfurtner CQG(05)gq/04 [Kerr, equatorial]; Cadoni CQG(05) [2D]; Cadoni & Mignemi PRD(05)gq [with singular source].
@ Back-reaction: Balbinot et al PRL(05)gq/04, PRD(05)gq/04, NCB(06)gq; Fagnocchi gq/06-in, gq/06-in.
@ Thermodynamics: Kim et al JKPS(06)gq/05 [entropy and superradiance].
@ Quasinormal modes: Berti et al PRD(04); Cardoso et al PRD(04) [rotating]; Lepe & Saavedra PLB(05) [and area spectrum]; Saavedra MPLA(06)gq/05; Abdalla et al CQG(07)-a0706 [Laval nozzles].
@ Other topics: Liberati et al CQG(00)gq [surface gravity]; Schützhold & Unruh PRD(02)gq [gravity waves]; Rosquist GRG(04)gq/03 [and electromagnetic waves]; Choy et al PRD(06) [superradiant energy flow].
@ In Bose-Einstein condensates: Garay et al PRL(00)gq, PRA(01)gq/00; Barceló et al CQG(01)gq/00, IJMPA(03)gq/01 [black hole radiation]; Visser et al ht/01-in; Weinfurtner gq/04-MS; Carusotto et al a0803 [radiation, numerical].
@ Laval nozzles: Furuhashi et al CQG(06)gq; Okuzumi & Sakagami gq/07 [quasinormal ringing, simulations].

For Electromagnetic Waves > s.a. light [optical].
@ References: Reznik PRD(00)gq/97 [radiation]; Schäfer & Sauerbrey ap/98 [high-intensity lasers]; Schützhold et al PRL(02)qp/01 [dielectrics]; Unruh & Schützhold PRD(03)gq [slow light]; Philbin et al a0711, a0711 + news pw(08)mar [event horizon in optical fibers].

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Send feedback and suggestions to bombelli at olemiss.edu – Modified 7 jul 2008