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| The '''Immirzi parameter''' (also known as the '''Barbero-Immirzi parameter''') is a numerical [[coefficient]] appearing in [[loop quantum gravity]], a nonperturbative theory of [[quantum gravity]]. The Immirzi parameter measures the size of the quantum of area in [[Planck units]].<ref name="rovelli">{{cite book|last=Rovelli|first=Carlo|title=Quantum Gravity|url=http://www.cpt.univ-mrs.fr/~rovelli/book.pdf|accessdate=2010-09-25|series=Cambridge Monographs on Mathematical Physics|year=2004|publisher=Cambridge University Press|location=Cambridge, UK|isbn=0-521-83733-2 }}</ref> As a result, its value is currently fixed by matching the semiclassical [[black hole entropy]], as calculated by [[Stephen Hawking]], and the counting of microstates in loop quantum gravity.
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| ==The reality conditions==
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| The Immirzi parameter arises in the process of expressing a Lorentz connection with noncompact group SO(3,1) in terms of a complex connection with values in a compact group of rotations, either SO(3) or its double cover SU(2). Although named after Giorgio Immirzi, the possibility of including this parameter was first pointed out by Fernando Barbero. The significance of this parameter remained obscure until the spectrum of the [[Volume operator|area operator]] in LQG was calculated. It turns out that the area spectrum is proportional to the Immirzi parameter.
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| ==Black hole thermodynamics==
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| In the 1970s Stephen Hawking, motivated by the analogy between the law of increasing area of black hole [[event horizon]]s and the [[second law of thermodynamics]], performed a [[Semiclassical gravity|semiclassical]] calculation showing that black holes are in [[thermodynamic equilibrium|equilibrium]] with [[thermal radiation]] outside them, and that black hole entropy (that is, the entropy of the radiation in equilibrium with the black hole) equals
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| :<math>\, S=A/4\!</math> (in [[Planck units]])
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| In 1997, [[Abhay Ashtekar|Ashtekar]], [[John Baez|Baez]], [[Alejandro Corichi|Corichi]] and [[Kirill Krasnov|Krasnov]] quantized the classical [[phase space]] of the exterior of a black hole in vacuum [[General Relativity]].<ref name="Ashtekar1997">{{cite journal |last=Ashtekar |first=Abhay |authorlink= |coauthors=Baez, John; Corichi, Alejandro; Krasnov, Kirill |year=1998 |month= |title=Quantum Geometry and Black Hole Entropy |journal=Physical Review Letters |volume=80 |issue=5 |pages=904–907 |id= |doi=10.1103/PhysRevLett.80.904 |url= |accessdate= |quote= |arxiv=gr-qc/9710007 |bibcode=1998PhRvL..80..904A}}</ref> They showed that the geometry of spacetime outside a black hole is described by [[spin network]]s, some of whose [[edge (graph theory)|edge]]s puncture the event horizon, contributing area to it, and that the quantum geometry of the horizon can be described by a [[U(1)]] [[Chern-Simons theory]]. The appearance of the group U(1) is explained by the fact that two-dimensional geometry is described in terms of the [[Rotation (mathematics)|rotation group]] SO(2), which is isomorphic to U(1). The relationship between area and rotations is explained by [[Girard's theorem]] relating the area of a [[spherical triangle]] to its angular excess.
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| By counting the number of spin-network states corresponding to an event horizon of area A, the entropy of black holes is seen to be
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|
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| :<math>\, S=\gamma_0 A/4\gamma.\!</math>
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| Here <math>\gamma </math> is the Immirzi parameter and either
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| :<math>\gamma_0=\ln(2) / \sqrt{3}\pi</math> | |
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| or
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| :<math>\gamma_0=\ln(3) / \sqrt{8}\pi,</math>
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| depending on the [[gauge group]] used in [[loop quantum gravity]]. So, by choosing the Immirzi parameter to be equal to <math>\,\gamma_0</math>, one recovers the [[Black hole thermodynamics|Bekenstein-Hawking entropy formula]]. This computation appears independent of the kind of black hole, since the given Immirzi parameter is always the same. However, Krzysztof Meissner<ref name="Meissner">{{cite journal |last=Meissner |first=Krzysztof A. |authorlink= |coauthors= |year=2004 |month= |title=Black-hole entropy in loop quantum gravity |journal=Classical and Quantum Gravity |volume=21 |issue= 22|pages=5245–5251 |id= |doi=10.1088/0264-9381/21/22/015 |url= |accessdate= |quote= |arxiv=gr-qc/0407052v1|bibcode = 2004CQGra..21.5245M }}</ref> and Marcin Domagala with Jerzy Lewandowski<ref name="Dogamala">{{cite journal |last=Domagala |first=Marcin |authorlink= |coauthors=Lewandowski, Jerzy |year=2004 |month= |title=Black-hole entropy from quantum geometry |journal=Classical and Quantum Gravity |volume=21 |issue= 22|pages=5233–5243 |id= |doi=10.1088/0264-9381/21/22/014 |url= |accessdate= |quote= |arxiv=gr-qc/0407051|bibcode = 2004CQGra..21.5233D }}</ref> have corrected the assumption that only the minimal values of the spin contribute. Their result involves the logarithm of a [[transcendental number]] instead of the logarithms of integers mentioned above.
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| The Immirzi parameter appears in the denominator because the entropy counts the number of edges puncturing the event horizon and the Immirzi parameter is proportional to the area contributed by each puncture.
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| ==Immirzi parameter in Spin Foam theory==
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| In late 2006, independent from the definition of [[isolated horizon]] theory, it was reported that in [[loop quantum gravity]] the eigenvalues of the [[Volume operator|area operator]] are symmetric by the [[ladder symmetry]].<ref name="Ansari2007">{{cite journal |last=Ansari |first=Mohammad H. |authorlink= |coauthors= |year=2007 |month= |title=Spectroscopy of a canonically quantized horizon |journal=[[Nuclear Physics B]] |volume=783 |issue=3 |pages=179–212 |id= |doi=10.1016/j.nuclphysb.2007.01.009 |url= |accessdate= |quote= |arxiv=hep-th/0607081|bibcode = 2007NuPhB.783..179A }}</ref> Corresponding to each eigenvalue there are a finite number of degenerate states.<ref name="Ansari2008">{{cite journal |last=Ansari |first=Mohammad H. |authorlink= |coauthors= |year=2008 |month= |title=Generic degeneracy and entropy in loop quantum gravity |journal=Nuclear Physics B |volume=795 |issue=3 |pages=635–644 |id= |doi=10.1016/j.nuclphysb.2007.11.038 |url= |accessdate= |quote= |arxiv=gr-qc/0603121|bibcode = 2008NuPhB.795..635A }}</ref> One application could be if the classical null character of a horizon is disregarded in the quantum sector, in the lack of energy condition and presence of gravitational propagation the Immirzi parameter tunes to:
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| :<math>\ln(3) / \sqrt{2} \pi, </math> | |
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| by the use of [[Olaf Dreyer]]'s conjecture for identifying the evaporation of minimal area cell with the corresponding area of the highly damping quanta. This proposes a kinematical picture for defining a quantum horizon via [[spin foam]] models, however the dynamics of such a model has not yet been studied.
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| ==Interpretation==
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| The parameter may be viewed as a renormalization of [[Newton's constant]]. Various speculative proposals to explain this parameter have been suggested: for example, an argument due to [[Olaf Dreyer]] based on [[quasinormal mode]]s.<ref name="Dreyer2003">{{cite journal |last=Dreyer |first=Olaf |authorlink= |coauthors= |year=2003 |month= |title=Quasinormal Modes, the Area Spectrum, and Black Hole Entropy |journal=Physical Review Letters |volume=90 |issue=8 |pages=081301 |id= |doi=10.1103/PhysRevLett.90.081301 |url= |accessdate= |quote= |pmid=12633415 |arxiv=gr-qc/0211076 |bibcode=2003PhRvL..90h1301D}}</ref>
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| Another more recent interpretation is that it is the measure of the value of [[parity (physics)|parity]] violation in quantum gravity,<ref name="Randono2006a">{{cite journal |last=Randono |first=Andrew |authorlink= |coauthors= |year=2006 |month= |title=Generalizing the Kodama State I: Construction |journal=ArΧiv e-print |volume= |issue= |pages= 11073|id= |url= |accessdate= |quote= |arxiv=gr-qc/0611073|bibcode = 2006gr.qc....11073R }}</ref><ref name="Randono2006b">{{cite journal |last=Randono |first=Andrew |authorlink= |coauthors= |year=2006 |month= |title=Generalizing the Kodama State II: Properties and Physical Interpretation |journal= ArΧiv e-print |volume= |issue= |pages= 11074|id= |url= |accessdate= |quote= |arxiv=gr-qc/0611074|bibcode = 2006gr.qc....11074R }}</ref> and its positive real value is necessary for the [[Kodama state]] of loop quantum gravity. As of today, no alternative calculation of this constant exists. If a second match with experiment or theory (for example, the value of Newton's force at long distance) were found requiring a different value of the Immirzi parameter, it would constitute evidence that loop quantum gravity cannot reproduce the physics of [[general relativity]] at long distances. On the other hand, the Immirzi parameter seems to be the only free parameter of vacuum LQG, and once it is fixed by matching one calculation to an "experimental" result, it could in principle be used to predict other experimental results. Unfortunately, no such alternative calculations have been made so far.
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| ==References==
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| {{Reflist|2}}
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| ==External links==
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| *[http://xxx.lanl.gov/abs/gr-qc/0005126 Quantum Geometry of Isolated Horizons and Black Hole Entropy], a calculation incorporating matter and the theory of [[isolated horizons]] from [[General Relativity]].
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| *[http://xxx.lanl.gov/abs/0711.1879 Area, Ladder Symmetry, and Degeneracy in Loop Quantum Gravity], a brief review on the quantum of [[area ladder symmetry]] and [[area degeneracy]] in [[loop quantum gravity]] and the application of these two in the calculation incorporating the modifications of [[black hole radiation]].
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| {{Black holes}}
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| [[Category:Black holes]]
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| [[Category:Loop quantum gravity]]
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