Asymptotics with a positive cosmological constant: I. Basic framework

Abstract

The asymptotic structure of the gravitational field of isolated systems has been analyzed in great detail in the case when the cosmological constant Λ is zero. The resulting framework lies at the foundation of research in diverse areas in gravitational science. Examples include: i) positive energy theorems in geometric analysis; ii) the coordinate invariant characterization of gravitational waves in full, non-linear general relativity; iii) computations of the energy-momentum emission in gravitational collapse and binary mergers in numerical relativity and relativistic astrophysics; and iv) constructions of asymptotic Hilbert spaces to calculate S-matrices and analyze the issue of information loss in the quantum evaporation of black holes. However, by now observations have established that Λ is positive in our universe. In this paper we show that, unfortunately, the standard framework does not extend from the Λ = 0 case to the Λ > 0 case in a physically useful manner. In particular, we do not have positive energy theorems, nor an invariant notion of gravitational waves in the non-linear regime, nor asymptotic Hilbert spaces in dynamical situations of semi-classical gravity. A suitable framework to address these conceptual issues of direct physical importance is developed in subsequent papers.

Induced gravity II: grand unification

“…In fact, it has been known for more than 30 years [17,18] that, to one-loop order, there are no unstable modes in de Sitter background provided the parameters of the model obey certain inequalities, which our present model satisfies. 31 To our knowledge, this has been most thoroughly investigated to by date by Ashtekar, Bonga, and Kesevan [38][39][40][41] who emphasize several distinct features of de Sitter space. No matter how small the cosmological constant, there are "no asymptotic Hilbert spaces in dynamical situations of semi-classical gravity" [39].…”

“…31 To our knowledge, this has been most thoroughly investigated to by date by Ashtekar, Bonga, and Kesevan [38][39][40][41] who emphasize several distinct features of de Sitter space. No matter how small the cosmological constant, there are "no asymptotic Hilbert spaces in dynamical situations of semi-classical gravity" [39]. Further, they show on physical grounds that one must include non-normalizable growing modes among the gravitational waves on I + .…”

Gravitational wave memory in de Sitter spacetime

“…In the appendix we show that these relations continue to hold. are contained in recent works of Ashtekar et al [19][20][21][22].…”

Slowly rotating perfect fluids with a cosmological constant

“…Definitions of a spacetime being asymptotically (anti)-de Sitter are given in [15,16], and we follow the notation given there. We can choose the conformal factorΩ 14) and also choose Λ such that |q 1 Λ| < 3.…”