Complex Kerr geometry and nonstationary Kerr solutions

Abstract

In the frame of the Kerr-Schild approach, we consider complex structure of the Kerr geometry which is determined by a complex world line of a complex source. The real Kerr geometry is represented as a real slice of this complex structure. The Kerr geometry is generalized to the nonstationary case when the current geometry is determined by a retarded time and is defined by a retarded-time construction via a given complex world line of source. A general exact solution corresponding to arbitrary motion of a spinning source is obtained. The acceleration of the source is accompanied by a lightlike radiation along the principal null congruence. It generalizes to the rotating case the known Kinnersley class of "photon rocket" solutions. PACS number(s): 04

Singularity-free model of electric charge in physical vacuum: non-zero spatial extent and mass generation

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“…A popular approach to the classical electron model was made using the Einstein-Dirac [18] and Kerr-Newman (KN) solutions [30][31][32][33][34][35][36][37][38][39][40][41][42] (an extensive bibliography can be found in [43]). While the original KN solution does have the correct gyromagnetic ratio, it also contains a naked singularity and thus requires an additional mechanism to circumvent the regularization problem; the story is far from being complete yet.…”

The Kerr Theorem and Multi-Particle Kerr–schild Solutions

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Instability of black hole horizon with respect to electromagnetic excitations

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“…The long-term attack on the DKS equations performed in [4,5,8,9, 10] has led to the obtained in [11] time-dependent solutions which revealed a holographic structure of the fluctuating Kerr-Schild spacetimes and showed explicitly that electromagnetic radiation from a black-hole interacting with vacuum contains two components: a) a set of the singular beam pulses (determined by function ψ(Y, τ ),) propagating along the Kerr PNC and breaking the topology and stability of the horizon; b)the regularized radiative component (determined by γ reg (Y, τ )) which is smooth and, similar to that of the the Vaidya 'shining star' solution [6], determines evaporation of the black-hole,…”