In this talk I will describe progresses in considering GR effects in the dynamics of structure formation. First I will present results of a nonlinear post-Friedman approximation, a kind of post-Newtonian formalism. Then I will focus on recent fully nonlinear numerical relativity simulations. Numerical relativity is a fundamental tool in the modelling of gravitational waves sources, but its...
I will talk about the GW signatures from the collisions of Oscillatons -- which are long-lived non-topological solutions of massive scalar fields. I will describe the technical challenges and present the GW wave forms of such collisions calculated using the numerical relativity code GRCHOMBO. I will show that for black hole end states, the total gravitational waves energy released in such...
The upcoming sub-millimetre VLBI images of Sgr A* by the EHT Collaboration are expected to provide critical evidence for the existence of this supermassive black hole. In the near future, strong field images could be used to test both deviations from General Relativity as well as different models for the compact object at the Galactic Centre. In this work we assess our present and future...
I will review the status of TEOBResumS, that is a state of the art effective-one-body based waveform model for spin-aligned coalescing compact binaries, e.g. black hole binaries and neutron star binaries. I will focus on the impact of the numerical relativity information needed to complete the analytical model and focus on the performance of the model for gravitational wave data-analytsis purposes.
An extended accelerating body under ‘rigid motion’ by definition manifests unvarying separation between its constituents in all comoving inertial frames. Relationships be- tween constituents’ necessarily di↵ering yet constant accelerations—reflecting a nonuni- form, dynamically changing and moreover repulsive gravitational field—have been es- tablished by Woodhouse in 2003 using Minkowski...
