Spherical Gravitational Waves

Some High-Frequency Gravitational Waves Related to Exact Radiative Spacetimes

“…The last equation in (17) can be put into the form d dl (ln A) = −Θ, where l is the affine parameter, and Θ = 1 2 k µ ;µ is the expansion of the null congruence. This determines the behaviour of the amplitude A in the above spacetimes (22), (31), (43). The remaining equations (17) enables one to deduce the polarization tensors.…”

“…The metric (generally of the Petrov type II) in the standard coordinates has the form, see e.g. [22,23,28,39],…”

“…then high-frequency gravitational waves (21), (22) introduce H which is given by equation (25). According to (27), the electromagnetic field is perturbed by the term proportional to h αβ h αβ = A 2 e 2iφ = O(ǫ 2 ), see (17), namely…”

“…Among the most important classes are planar pp -waves [17,18] which belong to a large family of non-expanding radiative spacetimes [19,20], cylindrical Einstein-Rosen waves [21], expanding "spherical" waves of the Robinson-Trautman type [22,23], spacetimes with boost-rotation symmetry representing radiation generated by uniformly accelerated sources [24,25,26], cosmological models of the Gowdy type [27], and others -for comprehensive reviews containing also a number of references see, e.g., [28,30,31,29,32].…”

Peeling properties of lightlike signals in general relativity

“…This is the conventional peeling behavior when compared with models of vacuum gravitational fields due to isolated gravitating systems in general (cf. [4]- [8] and (2.20)-(2.24) below). The purpose of the present paper is to explain the unconventional peeling behavior described above by putting it in the context of light-like signals emitted by a general class of isolated gravitating systems.…”