Mapping dynamical ejecta and disk masses from numerical relativity simulations of neutron star mergers. (arXiv:2011.11110v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Nedora_V/0/1/0/all/0/1">Vsevolod Nedora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schianchi_F/0/1/0/all/0/1">Federico Schianchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernuzzi_S/0/1/0/all/0/1">Sebastiano Bernuzzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Radice_D/0/1/0/all/0/1">David Radice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daszuta_B/0/1/0/all/0/1">Boris Daszuta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Endrizzi_A/0/1/0/all/0/1">Andrea Endrizzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perego_A/0/1/0/all/0/1">Albino Perego</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prakash_A/0/1/0/all/0/1">Aviral Prakash</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zappa_F/0/1/0/all/0/1">Francesco Zappa</a>

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 equations of state 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.

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 equations of state 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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