The zeroth law of thermodynamics says that the temperature of a system in thermodynamic equilibrium is constant. Its counterpart for black hole mechanics says that surface gravity of a weakly isolated horizon is constant. This result is non-trivial because the horizon geometry is not assumed to be spherically symmetric; the result holds even when the horizon itself is highly distorted so long as it is in equilibrium. It is established as follows.
Recall from Section 2.1.3 that the notion of surface gravity is tied to the choice of a null normal of the isolated horizon: . Now, using Equation (5) in Definition 2 (of WIHs), we obtain:: as emphasized above, the zeroth law holds even if the WIH is highly distorted and rapidly rotating.
If electromagnetic fields are included, one can also show that the electric potential is constant on the horizon . Finally, there is an interesting interplay between the zeroth law the action principle. Let us restrict ourselves to space-times which admit a non expanding horizon as inner boundary. Then the standard Palatini action principle is not well defined because the variation produces a non-vanishing surface term at the horizon. The necessary and sufficient condition for this surface term to vanish is precisely that the gravitational (and the electromagnetic) zeroth laws hold . Consequently, the standard action principle is well-defined if inner boundaries are WIHs.
In field theories, conserved quantities such as energy and angular momentum can be universally defined via a Hamiltonian framework: they are the numerical values of Hamiltonians generating canonical transformations corresponding to time translation and rotation symmetries. In absence of inner boundaries, it is this procedure that first led to the notion of the ADM energy and angular momentum at spatial infinity . At null infinity, it can also be used to define fluxes of Bondi energy and angular momentum across regions of , and values of these quantities associated with any cross-section of [17, 185].
This procedure can be extended to allow inner boundaries which are WIHs. The first ingredient required for a Hamiltonian framework is, of course, a phase space. The appropriate phase space now consists of fields living in a region of space-time outside the black hole, satisfying suitable boundary conditions at infinity and horizon. Let be the region of space-time that we are interested in. The boundary of consists of four components: the time-like cylinder at spatial infinity, two space-like surfaces and which are the future and past boundaries of , and an inner boundary which is to be the WIH (see Figure 6). At infinity, all fields are assumed to satisfy the fall-off conditions needed to ensure asymptotic flatness. To ensure that is a type II horizon, one fixes a rotational vector field on and requires that physical fields on are such that the induced geometry on is that of a type II horizon with as the rotational symmetry.
Two Hamiltonian frameworks are available. The first uses a covariant phase space which consists of the solutions to field equations which satisfy the required boundary conditions [25, 14]. Here the calculations are simplest if one uses a first order formalism for gravity, so that the basic gravitational variables are orthonormal tetrads and Lorentz connections. The second uses a canonical phase space consisting of initial data on a Cauchy slice of . In the gravitational sector, this description is based on the standard ADM variables. Since the conceptual structure underlying the main calculation and the final results are the same, the details of the formalism are not important. For definiteness, in the main discussion, we will use the covariant phase space and indicate the technical modifications needed in the canonical picture at the end.
The phase space is naturally endowed with a (pre-)symplectic structure – a closed 2-form (whose degenerate directions correspond to infinitesimal gauge motions). Given any two vector fields (i.e., infinitesimal variations) and on , the action of the symplectic 2-form on them provides a function on . A vector field on is said to be a Hamiltonian vector field (i.e., to generate an infinitesimal canonical transformation) if and only if . Since the phase space is topologically trivial, it follows that this condition holds if and only if there is a function on such that for all vector fields . The function is called a Hamiltonian and its Hamiltonian vector field; alternatively, is said to generate the infinitesimal canonical transformation .
Since we are interested in energy and angular momentum, the infinitesimal canonical transformations will correspond to time translations and rotations. As in any generally covariant theory, when the constraints are satisfied, values of Hamiltonians generating such diffeomorphisms can be expressed purely as surface terms. In the present case, the relevant surfaces are the sphere at infinity and the spherical section of the horizon. Thus the numerical values of Hamiltonians now consist of two terms: a term at infinity and a term at the horizon. The terms at infinity reproduce the ADM formulas for energy and angular momentum. The terms at the horizon define the energy and angular momentum of the WIH.
Let us begin with angular momentum (see  for details). Consider a vector field on which satisfies the following boundary conditions: (i) At infinity, coincides with a fixed rotational symmetry of the fiducial flat metric; and, (ii) on , it coincides with the vector field . Lie derivatives of physical fields along define a vector field on . The question is whether this is an infinitesimal canonical transformation, i.e., a generator of the phase space symmetry. As indicated above, this is the case if and only if there exists a phase space function satisfying:
Now, a direct calculation  shows that, in absence of gauge fields on , one has:local to the horizon and is not required to be a Killing field of the space-time metric even in a neighborhood of the horizon. Therefore, can be calculated knowing only the horizon geometry of a type II horizon.
We conclude our discussion of angular momentum with some comments:
To obtain an expression of the horizon energy, one has to find the Hamiltonian on generating diffeomorphisms along a time translation symmetry on . To qualify as a symmetry, at infinity must approach a fixed time translation of the fiducial flat metric. At the horizon, must be an infinitesimal symmetry of the type II horizon geometry. Thus, the restriction of to should be a linear combination of a null normal and the axial symmetry vector ,
However there is subtlety: Unlike in the angular momentum calculation where is required to approach a fixed rotational vector on , the restriction of to can not be a fixed vector field. For physical reasons, the constants and should be allowed to vary from one space-time to another; they are to be functions on phase space. For instance, physically one expects to vanish on the Schwarzschild horizon but not on a generic Kerr horizon. In the terminology of numerical relativity, unlike , the time translation must be a live vector field. As we shall see shortly, this generality is essential also for mathematical reasons: without it, evolution along will not be Hamiltonian!
At first sight, it may seem surprising that there exist choices of evolution vector fields for which no Hamiltonian exists. But in fact this phenomenon can also happen in the derivations of the ADM energy for asymptotically flat space-times in the absence of any black holes. Standard treatments usually consider only those that asymptote to the same unit time translation at infinity for all space-times included in the phase space. However, if we drop this requirement and choose a live which approaches different asymptotic time-translations for different space-times, then in general there exists no Hamiltonian which generates diffeomorphisms along such a . Thus, the requirement that the evolution be Hamiltonian restricts permissible . This restriction can be traced back to the fact that there is a fixed fiducial flat metric at infinity. At the horizon, the situation is the opposite: The geometry is not fixed and this forces one to adapt to the space-time under consideration, i.e., to make it live.
Apart from this important caveat, the calculation of the Hamiltonian is very similar to that for angular momentum. First, one evaluates the 1-form on whose action on any tangent vector field is given byHamiltonian vector field in phase space. It is Hamiltonian if and only if there is a phase space function – the would be energy of the WIH – satisfying
Let us analyze Equation (36). Clearly, a necessary condition for existence of is just the integrability requirementpermissible time evolution vector field. Since Equation (36) is precisely the first law of black hole mechanics, is permissible if and only if the first law holds. Thus the first law is the necessary and sufficient condition that the evolution generated by is Hamiltonian!
There are infinitely many permissible vector fields . To construct them, one can start with a suitably regular function of and , find so that , solve Equation (37) to obtain , and find a permissible with on . Each permissible defines a horizon energy and provides a first law (36). A question naturally arises: Can one select a preferred or, alternatively, a canonical function ? Now, thanks to the no-hair theorems, we know that for each choice of , there is precisely one stationary black hole in vacuum general relativity: the Kerr solution. So, it is natural to set , or, more explicitly,horizon mass: derived using a systematic Hamiltonian framework, following the same overall procedure that leads to the definition of the ADM 4-momentum at spatial infinity. Finally, note that the quantities which enter the first law refer just to physical fields on the horizon; one does not have to go back and forth between the horizon and infinity.
We will conclude with three remarks:
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