Mario Spera

A fully parallel, high precision, N-body code running on hybrid computing platforms

We present a new implementation of the numerical integration of the classical, gravitational, N-body problem based on a high order Hermites integration scheme with block time steps, with a direct evaluation of the particle-particle forces. The main innovation of this code (called HiGPUs) is its full parallelization, exploiting both OpenMP and MPI in the use of the multicore Central Processing Units as well as either Compute Unified Device Architecture (CUDA) or OpenCL for the hosted Graphic Processing Units. We tested both performance and accuracy of the code using up to 256GPUs in the supercomputer IBM iDataPlex DX360M3 Linux Infiniband Cluster provided by the Italian supercomputing consortium CINECA, for values of N=<8millions. We were able to follow the evolution of a system of 8million bodies for few crossing times, task previously unreached by direct summation codes.

Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code

Understanding the link between massive (

A Performance Comparison of Different Graphics Processing Units Running Direct N-Body Simulations

\gtrsim 30

Do open star clusters evolve towards energy equipartition

M

Hierarchical black hole triples in young star clusters: impact of Kozai-Lidov resonance on mergers

_{\odot{}}

Brownian motion of massive black hole binaries and the final parsec problem

) stellar black holes (BHs) and their progenitor stars is a crucial step to interpret observations of gravitational-wave events. In this paper, we discuss the final fate of very massive stars (VMSs), with zero-age main sequence (ZAMS) mass

Dynamics of tidally captured planets in the Galactic Center

>150

The formation and coalescence sites of the first gravitational wave events

M

Star cluster disruption by a massive black hole binary

_{\odot}

The interaction between supermassive black holes and globular clusters

, accounting for pulsational pair-instability supernovae (PPISNe) and for pair-instability supernovae (PISNe). We describe an updated version of our population synthesis code SEVN, in which we added stellar evolution tracks for VMSs with ZAMS mass up to