On the quantization of general relativity in anholonomic variables

In discussing Bohr-Sommerfeld-like quantum rules for gravity, it is argued that Einstein's Riemannian theory of general relativity rather leads to a quantum field-mechanics than to a quantum-field theory of gravity. We construct the canonically conjugate coordinates and momenta of this gravito-dynamics in the framework of the Einstein-Cartan teleparallelism.     

Center of mass integral in canonical general relativity

For a two-surface B tending to an infinite-radius round sphere at spatial infinity, we consider the Brown-York boundary integral H_B belonging to the energy sector of the gravitational Hamiltonian. Assuming that the lapse function behaves as N∼1 in the limit, we find agreement between H_B and the total Arnowitt-Deser-Misner energy, an agreement first noted by Braden, Brown, Whiting, and York. However, we argue that the Arnowitt-Deser-Misner mass-aspect differs from a gauge invariant mass-aspect by a pure divergence on the unit sphere. We also examine the boundary integral H_B corresponding to the Hamiltonian generator of an asymptotic boost, in which case the lapse N∼x^k grows like one of the asymptotically Cartesian coordinate functions. Such a two-surface integral defines the kth component of the center of mass for (the initial data belonging to) a Cauchy surface Σ bounded by B. In the large-radius limit, we find agreement between H_B and an integral introduced by Beig and Murchadha as an improvement upon the center-of-mass integral first written down by Regge and Teitelboim. Although both H_B and the Beig- Murchadha integral are naively divergent, they are in fact finite modulo the Hamiltonian constraint. Furthermore, we examine the relationship between H_B and a certain two-surface integral which is linear in the spacetime Riemann curvature tensor. Similar integrals featuring the curvature appear in works by Ashtekar and Hansen, Penrose, Goldberg, and Hayward. Within the canonical 3+1 formalism, we define gravitational energy and center of mass as certain moments of Riemann curvature.     

Canonical quantization of general relativity in discrete space-times

It has long been recognized that lattice gauge theory formulations, when applied to general relativity, conflict with the invariance of the theory under diffeomorphisms. We analyze discrete lattice general relativity and develop a canonical formalism that allows one to treat constrained theories in Lorentzian signature space-times. The presence of the lattice introduces a "dynamical gauge" fixing that makes the quantization of the theories conceptually clear, albeit computationally involved. The problem of a consistent algebra of constraints is automatically solved in our approach. The approach works successfully in other field theories as well, including topological theories. A simple cosmological application exhibits quantum elimination of the singularity at the big bang.     

Consistent canonical quantization of a model field theory with Schwinger term

Canonical quantization of a finite two-dimensional model field theory is consistently carried out, in spite of the occurrence of a non-canonical Schwinger term. Heisenberg field operators are defined perturbatively by means of the dimensionally regularized Feynman chronological product, while their equal-time commutators may be related to free-field equal-time commutators through the use of the non-covariant Dyson chronological product. A concrete agreement (including the axial anomaly) is thus found between the quantum Lagrangian and Hamiltonian formulations.     

Monad method and canonical formalism of general relativity

In this note the general monad method is systematically represented, and it is shown how it may be reduced to its two basic special gauges. The last section deals with two kinds of canonical formalism, coordinate and referential ones, based on the kinemetric gauge.     

Geometric interpretation of chronometric invariants in general theory of relativity

The geometric interpretation of Zelmanov's Chronometric invarians is given and their conection to observable quantities as well as the connection of Zelmanov's approach to the generally covariant Dehnen's method is found.The authors would like to thank Dr. J. Biák from the Dept. of Theoretical Physics, Charles University in Prague, for discussion and critical remarks.     

The canonical Lagrangian approach to three-space general relativity

We study the action for the three-space formalism of general relativity, better known as the Barbour–Foster–Ó Murchadha action, which is a square-root Baierlein–Sharp–Wheeler action. In particular, we explore the (pre)symplectic structure by pulling it back via a Legendre map to the tangent bundle of the configuration space of this action. With it we attain the canonical Lagrangian vector field which generates the gauge transformations (3-diffeomorphisms) and the true physical evolution of the system. This vector field encapsulates all the dynamics of the system. We also discuss briefly the observables and perennials for this theory. We then present a symplectic reduction of the constrained phase space.     

A canonical dynamics view of the Newtonian limit of general relativity

The Newtonian limit of general relativity was Jürgen Ehlers favourite model for limit relations between theories of physics. In this contribution, for the case of isolated systems, the Newtonian limit of general relativity will be illuminated from a canonical dynamics point of view. The canonical dynamics approach naturally supplies a post-Newtonian expansion of general relativity.     

Linking covariant and canonical general relativity via local observers

Hamiltonian gravity, relying on arbitrary choices of ‘space,’ can obscure spacetime symmetries. We present an alternative, manifestly spacetime covariant formulation that nonetheless distinguishes between ‘spatial’ and ‘temporal’ variables. The key is viewing dynamical fields from the perspective of a field of observers—a unit timelike vector field that also transforms under local Lorentz transformations. On one hand, all fields are spacetime fields, covariant under spacetime symmeties. On the other, when the observer field is normal to a spatial foliation, the fields automatically fall into Hamiltonian form, recovering the Ashtekar formulation. We argue this provides a bridge between Ashtekar variables and covariant phase space methods. We also outline a framework where the ‘space of observers’ is fundamental, and spacetime geometry itself may be observer-dependent.     

Application of the method of kinemetric invariants to the Cauchy problem in general relativity

A class of metrics in which the spatial part describes flat space is considered. The algebraic condition of reduction of the three-dimensional part of an arbitrary metric to Cartesian form is found. The Cauchy problem for these metrics is considered in terms of kinemetrically invariant quantities. The results are used to solve the Cauchy problem for a spherically symmetric gravitational field. A solution is also obtained for the tachyon twin of the Schwarzschild field.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 4, pp. 48–52, April, 1976.     

Generalization of general relativity to the space of closed strings

A geometrical string field theory is constructed on the space of bosonic closed strings. Einstein gravity is reproduced in a part of the massless sector at the level of the classical lagrangian.     

Relativistic canonical formalism and the invariant single-particle distribution function in the general theory of relativity

The relativistic canonical formalism is used to construct an eight-dimensional phase space and an invariant distribution function, and integral and differential operations in the phase space and statistical averages, associated with the field of geodesic observers, are introduced. Liouville's theorem is proved.     

Covariant canonical quantization of the green-schwarz superstring

Introducing a new type of D = 10 harmonic superspace with two generations of harmonic coordinates, we reduce the Green-Schwarz (GS) superstring to a system whose constraints are Lorentz covariant and functionally independent. These features allow us to impose Lorentz-covariant gauge fixing conditions for the reparametrization and the fermionic κ-invariances. The resulting Q_BRST corresponds to the finite-dimensional Lie algebra of the remaining purely harmonic constraints. The super-Poincaré symmetry acts in a manifestly Lorentz-covariant form and is apparently anomaly free.     

Kinks in general relativity

The problem of classifying topologically distinct general relativistic metrics is discussed. For a wide class of parallelizable space-time manifolds it is shown that a certain integer-valued topological invariant n always exists, and that quantization when n is odd will lead to spinor wave functionals.     

Time in general relativity

In order to distinguish between physical and coordinate effects in an arbitrary gravitational field, the space coordinate system and the clock rates must be specified operationallya priori. Once this is done, it is no longer possible to set up an initial surface arbitrarily, since this operation must be consistent with certain physical experiments, whose results depend upon the particular physical situation. A method is given for setting up the initial surface, and the time evolution of the system is discussed.NASA Predoctoral Fellow.     

Nonstandard canonical quantization of local field theories

A recent new approach to classical local field theories (CLFT) offers a new, alternative quantization procedure of fields. A brief discussion of this nonstandard field quantization is given.Presented at the International Conference Selected Topics in Quantum Field Theory and Mathematical Physics, Bechyn, Czechoslovakia, June 23–27, 1986.     

Tachyons in general relativity

The tachyonic version of the Schwarzschild (bradyonic) gravitational field within the framework of extended relativity is considered. The metric of a tachyonic black hole is obtained through superluminal transformations from a bradyonic metric. The extended space-time manifold of this geometry which includes both black and white tachyonic holes is analysed, and the differences between the tachyonic and bradyonic versions are noted. It is shown that the meanings of black holes, tachyons and bradyons depend on the character of the reference frame and are not absolute.