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

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...

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Published in:Classical and quantum gravity 2021-12, Vol.39 (1)
Main Authors: Nedora, Vsevolod, Schianchi, Federico, Bernuzzi, Sebastiano, Radice, David, Daszuta, Boris, Endrizzi, Andrea, Perego, Albino, Prakash, Aviral, Zappa, Francesco
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container_title Classical and quantum gravity
container_volume 39
creator Nedora, Vsevolod
Schianchi, Federico
Bernuzzi, Sebastiano
Radice, David
Daszuta, Boris
Endrizzi, Andrea
Perego, Albino
Prakash, Aviral
Zappa, Francesco
description 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.
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title Mapping dynamical ejecta and disk masses from numerical relativity simulations of neutron star mergers
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