We present a practical method for calculating the gravitational self-force, as well as the electromagnetic and scalar self-forces, for a particle in a generic orbit around a Kerr black hole. In particular, we provide the values of all the regularization parameters needed for implementing the (previously introduced) mode-sum regularization method. We also address the gauge-regularization problem...

We use high-resolution, three-dimensional hydrodynamics simulations to study the hydrodynamic and gravitational interaction between stellar companions embedded within a differentially rotating common envelope. Specifically, we evaluate the contributions of the non-axisymmetric gravitational tides and pressure forces to the drag force and, hence, to the dissipation rate and the mass accumulated ...

The aim of this study is to combine four fundamental forces in a single equation. Dirac equation is written by putting the Yukawa potential as a representation of the strong and gravitational forces. The ordinary terms seen in the Dirac Equation are treated as the representations of the electromagnetic forces. The Lagrangian of the weak local interaction of the charged particles is converted to...

The gravitational and electromagnetic fields of a moving charged spinning point particle are obtained in the Lorentz covariant form by transforming the Kerr–Newman solution in Boyer–Lindquist coordinates to the one in the coordinate system which resembles the isotropic coordinates and then covariantizing it. It is shown that the general relativistic proper time at the location of the particle i...

The conservative dephasing effects of gravitational self forces for extreme mass-ratio inspirals are studied. Both secular and non-secular conservative effects may have a significant effect on LISA waveforms that is independent of the mass ratio of the system. Such effects need to be included in generated waveforms to allow for accurate gravitational wave astronomy that requires integration tim...

Gravitational waves are propagating fluctuations of gravitational fields, that is, ”ripples” in spacetime, generated mainly by moving massive bodies. These distortions of spacetime travel with the speed of light. Every body in the path of such a wave feels a tidal gravitational force that acts perpendicular to the waves direction of propagation; these forces change the distance between points, ...

In this review we examine the dynamics and gravitational wave detectability of rotating strained neutron stars. The discussion is divided into two halves: triaxial stars, and precessing stars. We summarise recent work on how crustal strains and magnetic fields can sustain triaxiality, and suggest that Magnus forces connected with pinned superfluid vortices might contribute to deformation also. ...

Consider a binary star system (e.g., pulsar-white dwarf, pulsar-pulsar) with a significantly smaller companion, such as an exoplanet, in orbit about the binary. Given the absence of experimental data gathered within the vicinity of the binary, it is possible that the gravitational field within this system might not be accurately modeled by well-known pairwise gravitational forces. In this resea...

Background HA-TLS is very difficult to correct using other braces except for the Milwaukee brace (MB). Since the introduction of the MB, a major problem has been poor patient compliance due to the perception of the brace as cosmetically unacceptable. The forces applied to the spine by the MB are well illustrated by White-Panjabi (1). According to circadian biological rhythm, a sleeping person R...

Parametric resonance driven oscillations of a dumbbell satellite in elliptical orbit in central gravitational field of force under the combined effects of perturbing forces Earth Magnetic field and Oblateness of the Earth has been studied. The system comprises of two satellite connected by a light, flexible and inextensible cable, moves like a dumbbell satellite in elliptical orbit, in central ...