Conformal properties of nonpeeling vacuum spacetimes
Abstract
In a previous paper we investigated a class ofnonpeeling asymptotic vacuum solutions which were shown to admit finite expressions for the WinicourTamburino energymomentum and angular momentum integrals. These solutions have the property that ψ _0 = O(r^{  3  in _0 } ), in _0 ≤slant 2 and ψ _1 = O(r^{  3  in _1 } ), in _1< in _0 and in _1< 1 withψ _{2},ψ _{3}, andψ _{4} having the same asymptotic behavior as they do for peeling solutions. The above investigation was carried out in the physical spacetime. In this paper we examine the conformal properties of these solutions, as well as the more general CouchTorrence solutions, which include them as a subclass. For the CouchTorrence solutions begin{gathered} ψ _0 = O(r^{  2  in _0 } ) \ ψ _1 = O(r^{  2  in _1 } ), in _1< in _0 {text{ }}and in _1 ≤slant 2 \ and , ψ _2 = O(r^{  2  in _2 } ),{text{ }} in _2< in _1 {text{ }}and in _2 ≤slant 1 withψ _{3} andψ _{4} behaving as they do for peeling solutions. It is our purpose to determine how much of the structure generally associated with peeling spacetimes is preserved by the nonpeeling solutions. We find that, in general, a threedimensional null boundary (?^{+}) can be defined and that the BMS group remains the asymptotic symmetry group. For the general CouchTorrence solutions several physically and/or geometrically interesting quantities
 Publication:

General Relativity and Gravitation
 Pub Date:
 July 1982
 DOI:
 10.1007/BF00761457
 Bibcode:
 1982GReGr..14..655N