Simulating neutron stars with a flexible enthalpy-based equation of state parametrization in SpECTRE. (arXiv:2301.13818v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Legred_I/0/1/0/all/0/1">Isaac Legred</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_Y/0/1/0/all/0/1">Yoonsoo Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deppe_N/0/1/0/all/0/1">Nils Deppe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatziioannou_K/0/1/0/all/0/1">Katerina Chatziioannou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foucart_F/0/1/0/all/0/1">Francois Foucart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hebert_F/0/1/0/all/0/1">François Hébert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kidder_L/0/1/0/all/0/1">Lawrence E. Kidder</a>
Numerical simulations of neutron star mergers represent an essential step
toward interpreting the full complexity of multimessenger observations and
constraining the properties of supranuclear matter. Currently, simulations are
limited by an array of factors, including computational performance and input
physics uncertainties, such as the neutron star equation of state. In this
work, we expand the range of nuclear phenomenology efficiently available to
simulations by introducing a new analytic parametrization of cold,
beta-equilibrated matter that is based on the relativistic enthalpy. We show
that the new $textit{enthalpy parametrization}$ can capture a range of nuclear
behavior, including strong phase transitions. We implement the enthalpy
parametrization in the $texttt{SpECTRE}$, code, simulate isolated neutron
stars, and compare performance to the commonly used spectral and polytropic
parametrizations. We find comparable computational performance for nuclear
models that are well represented by either parametrization, such as simple
hadronic EoSs. We show that the enthalpy parametrization further allows us to
simulate more complicated hadronic models or models with phase transitions that
are inaccessible to current parametrizations.
Numerical simulations of neutron star mergers represent an essential step
toward interpreting the full complexity of multimessenger observations and
constraining the properties of supranuclear matter. Currently, simulations are
limited by an array of factors, including computational performance and input
physics uncertainties, such as the neutron star equation of state. In this
work, we expand the range of nuclear phenomenology efficiently available to
simulations by introducing a new analytic parametrization of cold,
beta-equilibrated matter that is based on the relativistic enthalpy. We show
that the new $textit{enthalpy parametrization}$ can capture a range of nuclear
behavior, including strong phase transitions. We implement the enthalpy
parametrization in the $texttt{SpECTRE}$, code, simulate isolated neutron
stars, and compare performance to the commonly used spectral and polytropic
parametrizations. We find comparable computational performance for nuclear
models that are well represented by either parametrization, such as simple
hadronic EoSs. We show that the enthalpy parametrization further allows us to
simulate more complicated hadronic models or models with phase transitions that
are inaccessible to current parametrizations.
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