On the exotic BTZ black holes Baocheng Zhang Based on papers PRL 110, 241302; PRD 88, 124017...
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Transcript of On the exotic BTZ black holes Baocheng Zhang Based on papers PRL 110, 241302; PRD 88, 124017...
On the exotic BTZ black holes
Baocheng ZhangBased on papers PRL 110, 241302; PRD 88, 124017
Coauthor: P. K. Townsend
KITPC, 2014-6-25
Outlines (2+1) dimensional gravity
BTZ black holes
Exotic BTZ black holes
Extension to BTZ BH in TMG
Discussion and Conclusion
Understand the classical gravity further Singularity; cosmic censorship; closed timelike
curves; ……
Gain an insight into quantum gravity Black hole solutions; gravitons (modified theory);
quantization; AdS/CFT correspondence; ……
(2+1) dimensional gravity
Why do we want to study (2+1) dimensional gravity?
(2+1) dimensional gravity 3D Einstein-Hilbert action can be written as
which is different from 4D action
And the former is equivalent to an ISO(2,1) Chern-Simons action, but there is not this equivalence for the latter. (Witten, 1988)
There are two essential features for vacuum gravity:• No local d.o.f. or propagating d.o.f. (Leutwyler, 1966)
• No black-hole solutions (Ida, 2000)
So it is usually considered as dynamics of flat space. (Deser, Jackiw, & t’Hooft, 1984)
(2+1) dimensional gravity
As discussed, (2+1) d GR doesn’t include the propagating d.o.f., but one can find some modified models to change the situation within which the physical spin-2 modes are massive.
3D massive gravity models includes: Topological massive gravity (Deser, Jackiw, & Templeton, 1982); New massive gravity (Bergshoeff, Hohm, & Townsend, 2009); General massive gravity (Bergshoeff, Hohm, & Townsend, 2009); Zwei-dreibein gravity (Bergshoeff, Haan, Hohm, Merbis, & Townsend,
2013); ……
(2+1) dimensional gravity
(2+1) dimensional gravity It is more interesting to consider the (2+1) d Einstein-
Hilbert action with a negative cosmological constant,
This model is the difference of two special linear group Chern-Simons terms, (Witten 1988)
Chern-Simons field equations is equivalent to vacuum Einstein field equations.
Outlines (2+1) dimensional gravity
BTZ black holes
Exotic BTZ black holes
Extension to BTZ BH in
Discussion and Conclusion
BTZ black holes There are no asymptotically flat black holes of 3D GR
but there are “BTZ” black holes, which are asymptotic to an AdS vacuum. (Banados, Teitelboim, & Zanelli, 1992)
The BTZ metric is locally isomorphic to the AdS vacuum, so any theory of 3D gravity admitting an AdS vacuum will also admit BTZ black holes.
Metric
Horizon
Mass and angular momentum (3D GR)
BTZ black holes The most important feature is that it has
thermodynamic properties analogous to (3+1) d black holes.
Temperature
Entropy
First/second/third laws
Inner mechanics (Detournay, 2012)
Bekenstein-Hawking entropy
State counting More important is to find the microscopic d.o.f.
responsible for the entropy which is beyond the thermodynamics given by classical gravity theory.
Chern-Simons description provides an effective way to approach the purpose.
Asymptotic symmetries and AdS/CFT (Brown & Henneaux)
Cardy formula (Cardy, 1986)
Effective central charge(see review by Carlip, 2005)
State counting For 3D GR, the central charges of dual CFT2 are
Using the Cardy formula and the relations
we get the entropies
The statistical mechanics demands the thermodynamic entropy of BTZ black holes (Strominger, 1998; Birmingham, et al, 1998)
What states are we counting? (see review by Carlip, 2005)
LS=S2R
rS
G
Outlines (2+1) dimensional gravity
BTZ black holes
Exotic BTZ black holes
Extension to BTZ BH in
Discussion and Conclusion
Exotic BTZ black holes BTZ metric solves any field equations that admit AdS as a
solution. For example, 3D conformal gravity. Mass M and angular momentum J of BTZ black holes given by
i.e. the reverse of 3D GR! The black hole is exotic.
Other 3D gravity models were earlier found to have the property. (Carlip & Gegenberg, 1991; Carlip et al, 1995; Banados, 1998)
Entropy of exotic BTZ black hole can be computed (e.g. by Wald formula) and is
The entropy is proportional to the area of inner horizon!
Non-BH entropy!
How should we understand the exotic black holes?
Why its mass and angular momentum interchange in the BTZ metric?
Exotic 3D EG 3D EG with AdS3 vacuum is a Chern-Simons theory for the
AdS3 group, that is, (Achucarro & Townsend, 1986)
The normal 3D EG is the difference of the two special linear group Chern-Simons terms. (Witten, 1988)
The sum gives a parity-odd “exotic” action with the same field equations (Witten, 1988). The Lagrangian 3-forms is,
where is torsion 2-form.
Exotic EG has exotic BH It was shown that 3D EG is equivalent to a Chern-Simons
gauge theory with the 1-form potential,
For every there is a conserved charge, defined as holonomy of asymptotic U(1) connection [CQG 12, 895 (1995)]
For normal 3D EG we have
For exotic 3D EG we have
So mass and angular momentum are reversed!
• For such exotic entropy, whether it still has the thermodynamic significance?
Thermodynamics The Hawking temperature and the angular momentum of BTZ
black hole are
which are geometrical and model-independent. For generality, consider the mass and angular momentum
It was shown that the only form of entropy
satisfies the first law of black hole thermodynamics
Note that the cases and correspond, respectively, to normal and exotic BTZ black holes.
Thermodynamics The event horizon is a Killing horizon for the Killing vector
At horizon, we have
which implies
For exotic BTZ black holes, it changes into
Through the calculation, we have the second law,
which means the SL is valid for the exotic BTZ black hole!
Such entropy was obtained before by the method of conical singularity (Solodukhin, 2006) and Wald’s Noether charge method extended to the case of parity-violation (Tachikawa, 2007).
For such exotic entropy, what is its microscopical interpretation through Cardy formula directly?
State counting
State counting For exotic 3D BTZ black hole, we have
The weak cosmic censorship condition
needed for the existence of the event horizon.
Thus we would have
which implies that Cardy formula would give an imaginary entropy.
The normal statistical mechanics is invalid!
A matter of convention Within thermodynamic approximation, the left and right
moving modes of CFT do not interact. This is exactly true if partition function of 3D Einstein gravity factorizes holomorphically: [Maloney & Witten, 2010]
Given factorization, we can change the conventions for left-moving modes, so that all energies are negative and all states have negative norm. This gives (which is known to be the case for conformal 3D gravity). Now we have
Appling the Cardy formula, we find
Exotic statistical mechanics Thermodynamics of exotic black holes is normal, so we expect
the formula
is still valid. So from the perspective of partition function, we have the
exotic statistical mechanics
in star contrast to the normal case
Now we have the entropy of exotic BTZ black hole
This is the thermodynamic entropy which is the first time to obtain the statistical exotic black hole entropy!
Outlines (2+1) dimensional gravity
BTZ black holes
Exotic BTZ black holes
Extension to BTZ BH in TMG
Discussion and Conclusion
Modified Cardy formulas Whether the modified Cardy formula can be
obtained with a fundamental method in CFT without recourse to the thermodynamic relation?
Using Carlip’s method to obtain
Cardy formula Partition function on a torus
Using modular invariance and saddle approxi., the density of states can be gotten as
If the central charge for the right mover is still positive, the same process led to the Cardy formula by taking the logarithm of the exponential term of the density of states; that is
Modified Cardy formula Now we begin to calculate the case with negative
central charge, and the density of states is
After using modular invariance, we have
Define
Using saddle point aproxi., the extremal point is
Modified Cardy formula Then the f function can be calculated as
The density of states
This leads to the modified Cardy formula,
Extension Topological massive gravity:
Its BTZ black hole solution:
Compared with NEG and EEG,
Identification of the parameters is dependent on concrete theories!
Extension Central charges: [Hotta, et al, 2008]
According to the previous modified Cardy formulas to calculate the entropy in different ranges of coupling parameter, we get a consistent form,
It is noticed that in the range
the entropy is negative, which is consistent with the range of negative mass.
Extension In previous calculation, we can get a term that gives the
logarithmic correction of entropy associated with the outer horizon,
For the 3D Einstein gravity, we obtain
For TMG, we obtain
This means that Chern-Simons term doesn’t influence the logarithmic correction of entropy
Outlines (2+1) dimensional gravity
BTZ black holes
Exotic BTZ black holes
Extension to BTZ BH in TMG
Discussion and Conclusion
Discussion Why BTZ black holes of conformal gravity are exotic
Negative central charge and holomorphic factorization
Area-Law; Higher-spin extension
S A A HS f y A
Extotic G Conformal Gtruncation
subgroup
Conclusions
The BTZ black holes of exotic 3D EG are exotic.
Thermodynamics of exotic black holes is normal.
Exotic black hole entropy needs exotic statistical mechanics.
Extension to TMG is feasible.