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Cauchy problem in spacetimes with closed timelike curves

Friedman, John and Morris, Michael S. and Novikov, Igor D. and Echeverria, Fernando and Klinkhammer, Gunnar and Thorne, Kip S. and Yurtsever, Ulvi (1990) Cauchy problem in spacetimes with closed timelike curves. Physical Review D, 42 (6). pp. 1915-1930. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:FRIprd90

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Abstract

The laws of physics might permit the existence, in the real Universe, of closed timelike curves (CTC’s). Macroscopic CTC’s might be a semiclassical consequence of Planck-scale, quantum gravitational, Lorentzian foam, if such foam exists. If CTC’s are permitted, then the semiclassical laws of physics (the laws with gravity classical and other fields quantized or classical) should be augmented by a principle of self-consistency, which states that a local solution to the equations of physics can occur in the real Universe only if it can be extended to be part of a global solution, one which is well defined throughout the (nonsingular regions of) classical spacetime. The consequences of this principle are explored for the Cauchy problem of the evolution of a classical, massless scalar field Φ (satisfying □Φ=0) in several model spacetimes with CTC’s. In general, self-consistency constrains the initial data for the field Φ. For a family of spacetimes with traversible wormholes, which initially possess no CTC’s and then evolve them to the future of a stable Cauchy horizon scrH, self-consistency seems to place no constraints on initial data for Φ that are posed on past null infinity, and none on data posed on spacelike slices which precede scrH. By contrast, initial data posed in the future of scrH, where the CTC’s reside, are constrained; but the constraints appear to be mild in the sense that in some neighborhood of every event one is free to specify initial data arbitrarily, with the initial data elsewhere being adjusted to guarantee self-consistent evolution. A spacetime whose self-consistency constraints have this property is defined to be ‘‘benign with respect to the scalar field Φ.’’ The question is posed as to whether benign spacetimes in some sense form a generic subset of all spacetimes with CTC’s. It is shown that in the set of flat, spatially and temporally closed, 2-dimensional spacetimes the benign ones are not generic. However, it seems likely that every 4-dimensional, asymptotically flat space-time that is stable and has a topology of the form R×(S-one point), where S is a closed 3-manifold, is benign. Wormhole spacetimes are of this type, with S=S^1×S^2. We suspect that these types of self-consistency behavior of the scalar field Φ are typical for noninteracting (linearly superposing), classical fields. However, interacting classical systems can behave quite differently, as is demonstrated by a study of the motion of a hard-sphere billiard ball in a wormhole spacetime with closed timelike curves: If the ball is classical, then some choices of initial data (some values of the ball’s initial position and velocity) give rise to unique, self-consistent motions of the ball; other choices produce two different self-consistent motions; and others might (but we are not yet sure) produce no self-consistent motions whatsoever. By contrast, in a path-integral formulation of the nonrelativistic quantum mechanics of such a billiard ball, there appears to be a unique, self-consistent set of probabilities for the outcomes of all measurements. This paper’s conclusion, that CTC’s may not be as nasty as people have assumed, is reinforced by the fact that they do not affect Gauss’s theorem and thus do not affect the derivation of global conservation laws from differential ones. The standard conservation laws remain valid globally, and in asymptotically flat, wormhole spacetimes they retain a natural, quasilocal interpretation.


Item Type:Article
Additional Information:©1990 The American Physical Society. Received 5 June 1990. For helpful discussions with one or another of us we thank Arley Anderson, Valery Frolov, Robert Geroch, Jonathan Halliwell, William Hiscock, James Hartle, Leonard Parker, Joe Polchinski, Carl Sagan, Edwin Salpeter, and Robert Wald. This research was supported in part by the National Science Foundation (Grants Nos. PHY-8603173 at the University of Wisconsin, and AST-8514911 and AST-8817792 at Caltech), by the Academy of Sciences of the USSR, and by the International Center for Theoretical Physics at Trieste.
Group:TAPIR
Record Number:CaltechAUTHORS:FRIprd90
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:FRIprd90
Alternative URL:http://dx.doi.org/10.1103/PhysRevD.42.1915
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:3737
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:11 Jul 2006
Last Modified:26 Dec 2012 08:56

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