scholarly journals Numerical relativity simulations of neutron star merger remnants using conservative mesh refinement

2015 ◽  
Vol 91 (12) ◽  
Author(s):  
Tim Dietrich ◽  
Sebastiano Bernuzzi ◽  
Maximiliano Ujevic ◽  
Bernd Brügmann
Keyword(s):  
Neutron Star ◽  
Numerical Relativity ◽  
Mesh Refinement

scholarly journals Aligned-spin neutron-star–black-hole waveform model based on the effective-one-body approach and numerical-relativity simulations

2020 ◽  
Vol 102 (4) ◽  
Author(s):  
Andrew Matas ◽  
Tim Dietrich ◽  
Alessandra Buonanno ◽  
Tanja Hinderer ◽  
Michael Pürrer ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Numerical Relativity ◽  
Model Based

scholarly journals Merger and Mass Ejection of Neutron Star Binaries

2019 ◽  
Vol 69 (1) ◽  
pp. 41-64 ◽  
Author(s):  
Masaru Shibata ◽  
Kenta Hotokezaka
Keyword(s):  
Numerical Simulation ◽  
Black Hole ◽  
Neutron Star ◽  
Numerical Relativity ◽  
High Energy ◽  
Ejection Process ◽  
Merger Process ◽  
Unique Approach ◽  
R Process ◽  
Mass Ejection

Mergers of binary neutron stars and black hole–neutron star binaries are among the most promising sources for ground-based gravitational-wave (GW) detectors and are also high-energy astrophysical phenomena, as illustrated by the observations of GWs and electromagnetic (EM) waves in the event of GW170817. Mergers of these neutron star binaries are also the most promising sites for r-process nucleosynthesis. Numerical simulation in full general relativity (numerical relativity) is a unique approach to the theoretical prediction of the merger process, GWs emitted, mass ejection process, and resulting EM emission. We summarize the current understanding of the processes of neutron star mergers and subsequent mass ejection based on the results of the latest numerical-relativity simulations. We emphasize that the predictions of the numerical-relativity simulations agree broadly with the optical and IR observations of GW170817.

scholarly journals Evolutions in 3D numerical relativity using fixed mesh refinement

2004 ◽  
Vol 21 (6) ◽  
pp. 1465-1488 ◽  
Author(s):  
Erik Schnetter ◽  
Scott H Hawley ◽  
Ian Hawke
Keyword(s):  
Numerical Relativity ◽  
Mesh Refinement

scholarly journals NUMERICAL RELATIVITY SIMULATIONS OF MAGNETIZED BLACK HOLE–NEUTRON STAR MERGERS

2015 ◽  
Author(s):  
ZACHARIAH B. ETIENNE ◽  
YUK TUNG LIU ◽  
VASILEIOS PASCHALIDIS ◽  
STUART L. SHAPIRO
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Numerical Relativity

scholarly journals Mapping dynamical ejecta and disk masses from numerical relativity simulations of neutron star mergers

2021 ◽  
Author(s):  
Vsevolod Nedora ◽  
Federico Schianchi ◽  
Sebastiano Bernuzzi ◽  
David Radice ◽  
Boris Daszuta ◽  
...  
Keyword(s):  
Comparative Analysis ◽  
Neutron Star ◽  
Equations Of State ◽  
Numerical Relativity ◽  
Mass Ratio ◽  
Quantitative Models ◽  
Neutrino Absorption

Abstract We present fitting formulae for the dynamical ejecta properties and remnant disk masses from the largest to date sample of numerical relativity simulations. The considered data include some of the latest simulations with microphysical nuclear equations of state (EOS) and neutrino transport as well as other results with polytropic EOS available in the literature. Our analysis indicates that the broad features of the dynamical ejecta and disk properties can be captured by fitting expressions, that depend on mass ratio and reduced tidal parameter. The comparative analysis of literature data shows that microphysics and neutrino absorption have a significant impact on the dynamical ejecta properties. Microphysical nuclear EOS lead to average velocities smaller than polytropic EOS, while including neutrino absorption results in larger average ejecta masses and electron fractions. Hence, microphysics and neutrino transport are necessary to obtain quantitative models of the ejecta in terms of the binary parameters.

GWs from compact binaries. Theory

2018 ◽  
Author(s):  
Michele Maggiore
Keyword(s):  
Neutron Star ◽  
Numerical Relativity ◽  
Compact Binaries

An introduction to recent analytic and numerical breakthroughs in the modelisation of the final phases of the coalescence of compact binaries. Effective one-body technique. Numerical relativity. Spinning binaries. Superkicks and recoil of the final BH. Astrophysical consequences. Coalescences of neutron-star binaries.

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