Thermodynamic Instabilities of Generalized Exotic BTZ Black Holes

TL;DR

This paper investigates the thermodynamic stability of generalized exotic BTZ black holes, challenging a previous conjecture by showing counterexamples where specific heat conditions do not align with the inequality.

Contribution

It provides the first counterexamples to the conjecture linking reverse isoperimetric inequality violation with negative specific heat in black holes.

Findings

Counterexamples where $C_V$ is positive despite inequality violation

All cases with positive $C_V$ have negative $C_P$, indicating instability

Broader conjecture may be necessary to describe black hole thermodynamics

Abstract

We examine the conjecture that black holes violating the reverse isoperimetric inequality have negative specific heat at constant volume $C_V$. We test this conjecture on the family of generalized exotic Ba\~nados, Teitelbiom and Zanelli (BTZ) black holes and find that $C_V$ can be positive even when the reverse isoperimetric inequality is violated, providing a counter example to the conjecture. However in all cases where $C_V$ is positive, the specific heat at constant pressure $C_P$ is negative, indicating that generalized exotic black holes are thermodynamically unstable, suggesting that a broader version of the conjecture might hold.

Equations

$$\mathcal{R}=\bigg{(}\frac{(d-1)V}{\omega_{d-2}}\bigg{)}^{\frac{1}{d-1}}\Big{(}\frac{\omega_{d-2}}{A}\Big{)}^{\frac{1}{d-2}}\geq 1$$

$$d{s}^2=-f(r)d{t}^2+\frac{1}{f(r)}d{r}^2+r^2(d\varphi -\frac{4j}{r^2}dt{)}^2$$

$$f(r)=-8m+\frac{r^2}{{\ell }^2}+\frac{16j^2}{r^2},$$

$$M=j/\ell ,J=\ell m.$$

$$M=\alpha m+\gamma \frac{j}{\ell },$$

$$J=\alpha j+\gamma \ell m$$

$$M$$

$$J$$

$$T$$

$$S$$

$$V$$

$$\mathcal{R}=\frac{1}{2}\sqrt{4\alpha -2\gamma \frac{r_{-}^3}{r_{+}^3}+6\gamma \frac{r_{-}}{r_{+}}}.$$

$$r_{E}\equiv\bigg{(}\frac{2J^{2}}{\pi P}\bigg{)}^{\frac{1}{4}}\leq r_{+}\leq\bigg{(}\frac{8J^{2}}{\pi P(1-\alpha)^{2}}\bigg{)}^{\frac{1}{4}}\;.$$

$$C_V=C_P-TV{\alpha }_T^2{\kappa }_T,$$

Full text

In the framework of extended black hole thermodynamics Kubiznak et al. (2017); Cvetic et al. (2011); Dolan (2011); Kastor et al. (2009); Caldarelli et al. (2000), the cosmological constant $\Lambda$ is interpreted as a pressure variable, $P=-\frac{\Lambda}{8\pi}$, whose variation leads to the extended first law, $dM=TdS+VdP$. Identifying the black hole mass $M$ as the enthalpy of the black hole, this looks like the usual first law of thermodynamics for systems with volume. The volume term $V$ in the extended first law is the conjugate potential to $P$, with $V=\frac{\partial M}{\partial P}|_{S}$. However this “volume” is not simply the geometric volume of the black hole except in simple cases such as the Anti-de Sitter (AdS) Schwarzchild black hole. Indeed, one need not even have a black hole present to define this volume; a single cosmological horizon is sufficient Mbarek and Mann (2017).

It has remained an ongoing puzzle to better understand the physical interpretation of this volume term. An early attempt to do so Cvetic et al. (2011) led to the conjecture that asymptotically AdS black holes satisfy the reverse isoperimetric inequality,

[TABLE]

for a $d-$dimensional spacetime. In this expression, $\omega_{d-2}$ is the dimensionless surface area of the unit ball in $d-1$ dimensions and $A$ is the surface area of the black hole horizon. The conjecture was motivated by the observation at the time that all known black holes seemed to respect the inequality (1). When the equality is saturated, a black hole of a given thermodynamic volues has attained its maximal possible entropy.

Since then, the isoperimetric ratio $\mathcal{R}$ of various black hole families have been studied, and some were found to violate this inequality Hennigar et al. (2015a); Klemm (2014); Hennigar et al. (2015b); Brenna et al. (2015); Noorbakhsh and Ghominejad (2017a, b); Feng et al. (2017); Noorbakhsh and Vahidinia (2018); Mann (2018). Such black holes have come to be called super-entropic, since they have more entropy that the relation (1) would admit.

What is still missing however is a physical interpretation of such violations. A recent proposal Johnson (2019a) hopes to remedy this shortfall by positing that violation of the reverse isoperimetric inequality implies a new type of thermodynamic instability, namely that the specific heat at constant volume, $C_{V}$, of the black hole will be negative. This was shown to be the case analytically for the $(2+1)$-dimensional charged Bañados, Teitelbiom and Zanelli BTZ black holes Banados et al. (1992) as well as numerically for the ultra spinning $d$-dimensional Kerr black hole Hennigar et al. (2015b). Systems with negative specific heat are unstable – an initial loss of energy is accompanied by an increase in temperature, leading to faster energy loss and a further increase in temperature. The system thus accelerates through this downward spiral rather than settling down to a nearby equilibrium state. In the case of black holes, this loss of energy can for example be due to Hawking Radiation. Traditionally, such instabilities were studied by looking at the sign of $C_{P}$, the specific heat at constant pressure. With the introduction of the volume term in extended thermodynamics it is natural to also look at $C_{V}$, which may harbour interesting physics Johnson (2019a, b).

Here we test the conjecture of Johnson (2019a) using the family of “generalized exotic BTZ black holes”, a term coined in Frassino et al. (2019). Such black holes violate the inequality (1) and so are superentropic. The relative simplicity of the spacetime makes them ideal candidates for studying their specific volumes and so testing the new instability conjecture. We find that generalized exotic BTZ black holes do not always have $C_{V}<0$, and so provide a counterexample to the conjecture. However we also find that whenever $C_{V}>0$ that $C_{P}<0$, indicating such black holes are in general thermodynamically unstable. This suggests a broader version of the instability conjecture: all super-entropic black holes are thermodynamically unstable.

A study of the thermodynamics of BTZ black holes Frassino et al. (2015) indicated that charged BTZ black holes were super-entropic. Generalized BTZ black holes are also super-entropic, but demonstration of this is somewhat more subtle. These objects are $(2+1)$-dimensional black holes whose metric is given by the usual rotating BTZ metric

[TABLE]

with

[TABLE]

where $\ell$ is the AdS radius. Here and below, we work with units in which $\hbar=G=c=k_{B}=1$. The roots of the function $f(r)$ give the inner and outer black hole horizons, $r_{\pm}=2\sqrt{\ell(\ell m\pm\sqrt{\ell^{2}m^{2}-j^{2}})}$. This metric is a solution to both the usual 3D Einstein action with a negative cosmological constant, as well as the parity-odd Einstein action Witten (1988). The expressions for the conserved mass $M$ and angular momentum $J$ as functions of the parameters $m$ and $j$ depend on the choice of action Carlip et al. (1995). In the former case $m$ and $j$ are respectively the mass and angular momentum of the black hole, while for the latter action we have the “exotic” case, with Townsend and Zhang (2013)

[TABLE]

This reversed role of the $m$ and $j$ parameters has also been found in other gravity models Carlip et al. (1995); Carlip and Gegenberg (1991); Bañados (1998); Bañados et al. (1998).

If one takes the gravitation action to be $I=\alpha I_{EH}+\gamma I_{GCS}$, which is a linear combination of the Einstein-Hilbert (EH) action and the gravitating Chern-Simons (GCS) action Frassino et al. (2019); Solodukhin (2006), then one obtains the generalized exotic BTZ black holes, for which

[TABLE]

are the conserved mass and angular momentum Frassino et al. (2019), with $\alpha\in(0,1)$ and $\gamma=1-\alpha$. When $\alpha=1$, we have the standard BTZ black hole while $\alpha=0$ corresponds to the exotic BTZ black hole.

The thermodynamic variables of the generalized exotic BTZ black holes are Frassino et al. (2019)

[TABLE]

They satisfy the first law, $dM=TdS+VdP+\Omega dJ$ as well as the Smarr relation, $0=TS-2PV+\Omega J$. The ratio $\mathcal{R}$ can be readily computed to be Frassino et al. (2019)

[TABLE]

The reverse isoperimetric inequality is saturated for standard BTZ black holes ($\alpha=1$) with $\mathcal{R}=1$. For all other $\alpha$ values, $\mathcal{R}\leq 1$ with equality if and only if $r_{-}=r_{+}$, i.e., the case of extremal black holes. Hence, the reverse isoperimetric inequality is violated for all generalized exotic BTZ black holes except for the standard BTZ and extremal cases. We thus expect these black holes to have negative specific heat according to the conjecture in Johnson (2019a).

We begin our study of thermodynamic stability by looking at the $C_{P}=T\frac{\partial S}{\partial T}|_{P,J}$ of generalized exotic BTZ black holes. Analytic expression of $C_{P}(r_{+},P,J)$ can be obtained by first solving for $r_{m}$ in terms of $(J,P,r_{+})$ using eq. 8, and then substituting this into the expressions for temperature, eq.  9, and entropy, eq. 10. We can then use the relation $\frac{\partial S}{\partial T}|_{P,J}=\frac{\partial S}{\partial r_{+}}|_{P,J}\frac{\partial r_{+}}{\partial T}|_{P,J}$ to find $C_{P}$.

The result is shown in fig. 1 (see also Frassino et al. (2019)). The range of $r_{+}$ on this figure is chosen to ensure $0\leq r_{m}\leq r_{+}$, which translates into the condition

[TABLE]

The black hole is extremal if $r_{+}=r_{-}=r_{E}$. For “more exotic” black holes i.e., $\alpha<1/2$ (solid curves) $C_{P}$ is negative except for extremal cases where it is zero while for more standard black holes ($\alpha>1/2$) $C_{P}$ is positive except again at $r_{+}=r_{E}$ where it is zero. Already, we are seeing that more exotic black holes are unstable according to the sign of $C_{P}$.

We now move on to look at $C_{V}$ for these black holes. To do this, we make use of the expression Johnson (2019a)

[TABLE]

where $\alpha_{p}\equiv V^{-1}\partial V/\partial T|_{P,J}$ and $\kappa_{T}\equiv-V\partial P/\partial V|_{T,J}$. Each of these expressions can be evaluated in a similar manner to $C_{P}$.

The result is shown in fig. 2. First, notice that $C_{V}$ of $1/2<\alpha<1$ (bottom figure) black holes are negative, in agreement with the conjecture in Johnson (2019a). When $\alpha=1$, $C_{V}=0$, as expected for the standard BTZ black hole. Recall that the $C_{P}$ of these black holes are non-negative. This thus illustrates how the thermodynamic stability of black holes depends on whether we are keeping $P$ or $V$ fixed.

More interesting is the $\alpha<1/2$ (top figure) case. When $\alpha$ is close to $1/2$, the $C_{V}$ remains negative, as in the red and green curve in the figure. These curves terminate at the extremal limit $r_{+}=r_{-}$. However, as the black hole becomes more exotic with decreasing $\alpha$, we see that $C_{V}$ can become positive at large enough $r_{+}$ as is the case for the blue, yellow, and purple ($\alpha=0$) curves. The divergences in $C_{V}$ occur whenever $\partial V/\partial P|_{T,J}=0$.

Summarizing, we have shown that generalized exotic BTZ black holes with a sufficiently small $\alpha$ parameter are counter-examples to the conjecture in Johnson (2019a): they violate the reverse isoperimetric inequality but possess positive $C_{V}$. However we note that an alternate (weaker) interpretation111We thank Clifford Johnson for pointing this out. of the conjecture might be that any connected branch of black holes that is super-entropic will have $C_{v}<0$ for at least some part of the branch and therefore the entire branch is thermodynamically unstable. While our results are consistent with this (weaker) interpretation, we regard it to be less precise since the meaning “connected branch” of black holes is somewhat ambiguous222For instance in the charged Schwarzschild-AdS solution, a single temperature can admit two black hole solutions at the same pressure and charge. These belong respectively to “small black hole” and “large black hole” solution branches (see for example Kubiznak and Mann (2012) for more details). Such distinctions do not occur in the generalized exotic BTZ case Frassino et al. (2019). However the divergence in $C_{v}$ can be argued to separate the class of exotic solutions into different branches..

We have also observed that $C_{P}<0$ whenever $C_{V}>0$. We therefore posit a further broader conjecture that black holes violating the reverse isoperimetric inequality will be thermodynamically unstable. It will be interesting to see if this broader conjecture can either be proven or if a counterexample can be found.

Acknowledgments

We would like to thank Antonia Micol Frassino and Jonas Mureika for helpful comments, and Clifford Johnson for helpful correspondence. This work was supported in part by the Natural Sciences and Engineering Research Council of Canada.