Open-source nuclear equation of state framework based on the liquid-drop model with Skyrme interaction

Schneider, A.; Roberts, Luke F.; Ott, Christian D.

doi:10.1103/physrevc.96.065802

Cited by 127 publications

(157 citation statements)

References 98 publications

(238 reference statements)

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“…Since we have sampled a few EOSs rather than working with an EOS family with free parameters (such a thing not being available for T,Y edependent EOSs until very recently [46]), we could not do such a search systematically, e.g., by fixing compaction and varying some independent variable. However, our lowmass soft EOS has compaction similar to our high-mass stiff EOS.…”

Section: Discussionmentioning

confidence: 99%

Black hole-neutron star mergers using a survey of finite-temperature equations of state

et al. 2018

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Each of the potential signals from a black hole-neutron star merger should contain an imprint of the neutron star equation of state: gravitational waves via its effect on tidal disruption, the kilonova via its effect on the ejecta, and the gamma-ray burst via its effect on the remnant disk. These effects have been studied by numerical simulations and quantified by semianalytic formulas. However, most of the simulations on which these formulas are based use equations of state without finite temperature and compositiondependent nuclear physics. In this paper, we simulate black hole-neutron star mergers varying both the neutron star mass and the equation of state, using three finite-temperature nuclear models of varying stiffness. Our simulations largely vindicate formulas for ejecta properties but do not find the expected dependence of disk mass on neutron star compaction. We track the early evolution of the accretion disk, largely driven by shocking and fallback inflow, and do find notable equation-of-state effects on the structure of this early-time, neutrino-bright disk.

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Section: Discussionmentioning

confidence: 99%

Black hole-neutron star mergers using a survey of finite-temperature equations of state

et al. 2018

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“…Amongst the validation binaries, we simulated the evo-lution of the long-lived remnant employing a microphysical EOS SLy4 [113] starting from a binary system of individual NS masses of 1.30 M at different resolutions. These simulations span six orbits before merger and last for more than 100 ms after merger.…”

Section: Appendix A: Quasiuniversal Relationsmentioning

confidence: 99%

Kilohertz gravitational waves from binary neutron star remnants: Time-domain model and constraints on extreme matter

et al. 2019

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The remnant star of a neutron star merger is an anticipated loud source of kiloHertz gravitational waves that conveys unique information on the equation of state of hot matter at extreme densities. Observations of such signals are hampered by the photon shot noise of ground-based interferometers and pose a challenge for gravitational-wave astronomy. We develop an analytical time-domain waveform model for postmerger signals informed by numerical relativity simulations. The model completes effective-one-body waveforms for quasi-circular nonspinning binaries in the kiloHertz regime. We show that a template-based analysis can detect postmerger signals with a minimal signal-to-noise ratios (SNR) of 8, corresponding to GW170817-like events for third-generation interferometers. Using Bayesian model selection and the complete inspiral-merger-postmerger waveform model it is possible to infer whether the merger outcome is a prompt collapse to a black hole or a remnant star. In the latter case, the radius of the maximum mass (most compact) nonrotating neutron star can be determined to kilometer precision. We demonstrate the feasibility of inferring the stiffness of the equation of state at extreme densities using the quasiuniversal relations deduced from numerical-relativity simulations.

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“…We use the meta-modeling formalism to construct a family of nite temperature EOSs of dense ma er. e EOSs are built using the recently developed open-source SROEOS code [12], which is itself based on the La imer and Swesty liquid-drop model of nuclei [13], with a few improvements. e main improvements relevant to this work are the possibility to compute EOSs where (1) the e ective mass of nucleons is di erent from their vacuum values and (2) for any desired value of the incompressibility of nuclear ma er K sat , instead of the canonical values of 180 MeV, 220 MeV, and 375 MeV to which the code of [13] is essentially limited.…”

Section: Introductionmentioning

confidence: 99%

Equation of state effects in the core collapse of a 20−M⊙ star

Schneider

Roberts

Ott³

et al. 2019

Phys. Rev. C

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Uncertainties in our knowledge of the properties of dense ma er near and above nuclear saturation density are among the main sources of variations in multi-messenger signatures predicted for core-collapse supernovae (CCSNe) and the properties of neutron stars (NSs). We construct 97 new nite-temperature equations of state (EOSs) of dense ma er that obey current experimental, observational, and theoretical constraints and discuss how systematic variations in the EOS parameters a ect the properties of cold nonrotating NSs and the core collapse of a 20-M progenitor star. e core collapse of the 20-M progenitor star is simulated in spherical symmetry using the general-relativistic radiation-hydrodynamics code GR1D where neutrino interactions are computed for each EOS using the NuLib library. We conclude that the e ective mass of nucleons at densities above nuclear saturation density is the largest source of uncertainty in the CCSN neutrino signal and dynamics even though it plays a subdominant role in most properties of cold NS ma er. Meanwhile, changes in other observables a ect the properties of cold NSs, while having li le e ect in CCSNe. To strengthen our conclusions, we perform six octant three-dimensional CCSN simulations varying the e ective mass of nucleons at nuclear saturation density. We conclude that neutrino heating and, thus, the likelihood of explosion is signi cantly increased for EOSs where the e ective mass of nucleons at nuclear saturation density is large.PACS numbers: 21.65. Mn,26.50.+x,26.60.Kp

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Open-source nuclear equation of state framework based on the liquid-drop model with Skyrme interaction

Cited by 127 publications

References 98 publications

Black hole-neutron star mergers using a survey of finite-temperature equations of state

Black hole-neutron star mergers using a survey of finite-temperature equations of state

Kilohertz gravitational waves from binary neutron star remnants: Time-domain model and constraints on extreme matter

Equation of state effects in the core collapse of a 20−M⊙ star

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