Self-action in Gravity

Abstract

On a particle moving with variable acceleration in the flat space-time affects the self-force due to outgoing radiation. The gravitational fields bring an additional contribution to self-force due to scattering waves on the curved backgrounds. This force is not zero even for a particle at rest. A review of the self-interaction in the gravitational field is presented. We consider the self-force for the particle connected with the vector and scalar fields. Different backgrounds are considered -black holes, stars, topological defects, and wormholes.

Electromagnetic self-force on a charged particle on Kerr spacetime: Equatorial circular orbits

“…Calculating the tail integral in practice is a technical challenge (though see [23]); fortunately, there are equivalent formulations available, as described in the review articles [21] and [24] (see also Ref. [25]). Prominent among these is the mode sum regularization (MSR) method introduced by Barack and Ori [26], which has been applied by numerous authors [27][28][29][30][31][32][33][34][35][36] for efficient and accurate calculations of the self-force.…”

Electromagnetic self-force on a charged particle on Kerr spacetime: equatorial circular orbits

“…Calculating the tail integral in practice is a technical challenge (though see [23]); fortunately, there are equivalent formulations available, as described in the review articles [21] and [24] (see also Ref. [25]). Prominent among these is the mode sum regularization (MSR) method introduced by Barack and Ori [26], which has been applied by numerous authors [27][28][29][30][31][32][33][34][35][36] for efficient and accurate calculations of the self-force.…”