20 research outputs found
Pair of null gravitating shells II. Canonical theory and embedding variables
The study of the two shell system started in our first paper ``Pair of null
gravitating shells I'' (gr-qc/0112060) is continued. An action functional for a
single shell due to Louko, Whiting and Friedman is generalized to give
appropriate equations of motion for two and, in fact, any number of spherically
symmetric null shells, including the cases when the shells intersect. In order
to find the symplectic structure for the space of solutions described in paper
I, the pull back to the constraint surface of the Liouville form determined by
the action is transformed into new variables. They consist of Dirac
observables, embeddings and embedding momenta (the so-called Kucha\v{r}
decomposition). The calculation includes the integration of a set of coupled
partial differential equations. A general method of solving the equations is
worked out.Comment: 20 pages, Latex file using amstex, some references correcte
Pair of null gravitating shells III. Algebra of Dirac's observables
The study of the two-shell system started in ``Pair of null gravitating
shells I and II'' (gr-qc/0112060--061) is continued. The pull back of the
Liouville form to the constraint surface, which contains complete information
about the Poisson brackets of Dirac observables, is computed in the singular
double-null Eddington-Finkelstein (DNEF) gauge. The resulting formula shows
that the variables conjugate to the Schwarzschild masses of the intershell
spacetimes are simple combinations of the values of the DNEF coordinates on
these spacetimes at the shells. The formula is valid for any number of in- and
out-going shells. After applying it to the two-shell system, the symplectic
form is calculated for each component of the physical phase space; regular
coordinates are found, defining it as a symplectic manifold. The symplectic
transformation between the initial and final values of observables for the
shell-crossing case is written down.Comment: 26 pages, Latex file using amstex, some references correcte
Pair of null gravitating shells I. Space of solutions and its symmetries
The dynamical system constituted by two spherically symmetric thin shells and
their own gravitational field is studied. The shells can be distinguished from
each other, and they can intersect. At each intersection, they exchange energy
on the Dray, 't Hooft and Redmount formula. There are bound states: if the
shells intersect, one, or both, external shells can be bound in the field of
internal shells. The space of all solutions to classical dynamical equations
has six components; each has the trivial topology but a non trivial boundary.
Points within each component are labeled by four parameters. Three of the
parameters determine the geometry of the corresponding solution spacetime and
shell trajectories and the fourth describes the position of the system with
respect to an observer frame. An account of symmetries associated with
spacetime diffeomorphisms is given. The group is generated by an infinitesimal
time shift, an infinitesimal dilatation and a time reversal.Comment: 28 pages, 9 figure included in the text, Latex file using amstex,
epic and graphi
Time evolution and observables in constrained systems
The discussion is limited to first-class parametrized systems, where the
definition of time evolution and observables is not trivial, and to finite
dimensional systems in order that technicalities do not obscure the conceptual
framework. The existence of reasonable true, or physical, degrees of freedom is
rigorously defined and called {\em local reducibility}. A proof is given that
any locally reducible system admits a complete set of perennials. For locally
reducible systems, the most general construction of time evolution in the
Schroedinger and Heisenberg form that uses only geometry of the phase space is
described. The time shifts are not required to be 1symmetries. A relation
between perennials and observables of the Schroedinger or Heisenberg type
results: such observables can be identified with certain classes of perennials
and the structure of the classes depends on the time evolution. The time
evolution between two non-global transversal surfaces is studied. The problem
is posed and solved within the framework of the ordinary quantum mechanics. The
resulting non-unitarity is different from that known in the field theory
(Hawking effect): state norms need not be preserved so that the system can be
lost during the evolution of this kind.Comment: 31 pages, Latex fil
Quantum Formation of Black Hole and Wormhole in Gravitational Collapse of a Dust Shell
Quantum-mechanical model of self-gravitating dust shell is considered. To
clarify the relation between classical and quantum spacetime which the shell
collapse form, we consider various time slicing on which quantum mechanics is
developed. By considering the static time slicing which corresponds to an
observer at a constant circumference radius, we obtain the wave functions of
the shell motion and the discrete mass spectra which specify the global
structures of spherically symmetric spacetime formed by the shell collapse. It
is found that wormhole states are forbidden when the rest mass is comparable
with Plank mass scale due to the zero-point quantum fluctuations.Comment: 10 pages in twocolumn, 8 figures, RevTeX 3.
Global phase time and path integral for string cosmological models
A global phase time is identified for homogeneous and isotropic cosmological
models yielding from the low energy effective action of closed bosonic string
theory. When the Hamiltonian constraint allows for the existence of an
intrinsic time, the quantum transition amplitude is obtained by means of the
usual path integral procedure for gauge systems.Comment: 12 pages, added reference
Gauge invariance of parametrized systems and path integral quantization
Gauge invariance of systems whose Hamilton-Jacobi equation is separable is
improved by adding surface terms to the action fuctional. The general form of
these terms is given for some complete solutions of the Hamilton-Jacobi
equation. The procedure is applied to the relativistic particle and toy
universes, which are quantized by imposing canonical gauge conditions in the
path integral; in the case of empty models, we first quantize the parametrized
system called ``ideal clock'', and then we examine the possibility of obtaining
the amplitude for the minisuperspaces by matching them with the ideal clock.
The relation existing between the geometrical properties of the constraint
surface and the variables identifying the quantum states in the path integral
is discussed.Comment: 23 page
Time and Time Functions in Parametrized Non-Relativistic Quantum Mechanics
The ``evolving constants'' method of defining the quantum dynamics of
time-reparametrization-invariant theories is investigated for a particular
implementation of parametrized non-relativistic quantum mechanics (PNRQM). The
wide range of time functions that are available to define evolving constants
raises issues of interpretation, consistency, and the degree to which the
resulting quantum theory coincides with, or generalizes, the usual
non-relativistic theory. The allowed time functions must be restricted for the
predictions of PNRQM to coincide with those of usual quantum theory. They must
be restricted to have a notion of quantum evolution in a time-parameter
connected to spacetime geometry. They must be restricted to prevent the theory
from making inconsistent predictions for the probabilities of histories.
Suitable restrictions can be introduced in PNRQM but these seem unlikely to
apply to a reparametrization invariant theory like general relativity.Comment: 18pages, 1postscript figure in separate file, uses REVTEX 3.
Global phase time and path integral for the Kantowski--Sachs anisotropic univers
The action functional of the anisotropic Kantowski--Sachs cosmological model
is turned into that of an ordinary gauge system. Then a global phase time is
identified for the model by imposing canonical gauge conditions, and the
quantum transition amplitude is obtained by means of the usual path integral
procedure of Fadeev and Popov.Comment: 11 page
Radiation reaction for multipole moments
We propose a Poincare-invariant description for the effective dynamics of
systems of charged particles by means of intrinsic multipole moments. To
achieve this goal we study the effective dynamics of such systems within two
frameworks -- the particle itself and hydrodynamical one. We give a
relativistic-invariant definition for the intrinsic multipole moments both
pointlike and extended relativistic objects. Within the hydrodynamical
framework we suggest a covariant action functional for a perfect fluid with
pressure. In the case of a relativistic charged dust we prove the equivalence
of the particle approach to the hydrodynamical one to the problem of radiation
reaction for multipoles. As the particular example of a general procedure we
obtain the effective model for a neutral system of charged particles with
dipole moment.Comment: 12 pages, 1 figure, RevTeX 4; references updated, minor textual
correction