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Building Neutron Stars with the MUSES Calculation Engine
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abstract
Exploring the equation of state of dense matter is an essential part of interpreting the observable properties of neutron stars. We present here the first results for dense matter in the zero-temperature limit generated by the MUSES Calculation Engine, a composable workflow management system that orchestrates calculation and data processing stages comprising a collection of software modules designed within the MUSES framework. The modules presented in this work calculate equations of state using algorithms spanning three different theories/models: (1) Crust Density Functional Theory, valid starting at low densities, (2) Chiral Effective Field Theory, valid around saturation density, and (3) the Chiral Mean Field model, valid beyond saturation density. Lepton contributions are added through the Lepton module to each equation of state, ensuring charge neutrality and the possibility of $\beta$-equilibrium. Using the Synthesis module, we match the three equations of state using different thermodynamic variables and different methods. We then couple the complete equation of state to a novel full-general-relativity solver (QLIMR) module that calculates neutron star properties. We find that the matching performed using different thermodynamic variables affects differently the range obtained for neutron star masses and radii (although never beyond a few percent difference). We also investigate the universality of equation of state-independent relations for our matched stars. Finally, for the first time, we use the Flavor Equilibration module to estimate bulk viscosity and flavor relaxation charge fraction and rates (at low temperature) for Chiral Effective Field Theory and the Chiral Mean Field model.
Forward citations
Cited by 7 Pith papers
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Neural-Accelerated Bayesian Calibration of Chiral Mean-Field Models to Nuclear Saturation and Vacuum Properties
A neural-accelerated Bayesian calibration of the chiral mean-field model shows that nuclear vacuum and saturation data constrain combinations of couplings while leaving individual parameters and neutron-star predictio...
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Highly-accurate neutron star modeling in the Hartle-Thorne Approximation
The Hartle-Thorne slow-rotation expansion is extended to seventh order, yielding analytical exterior metrics and multipole moments up to S7 for isolated neutron stars.
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Microscopic constraints for the equation of state and structure of neutron stars: a Bayesian model mixing framework
A Bayesian model mixing framework using Gaussian processes extends chiral EFT and pQCD constraints to neutron star matter and demonstrates kernel-dependent equation of state and mass-radius predictions.
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An Overview of the MUSES Calculation Engine and How It Can Be Used to Describe Neutron Stars
Matching the crust and core equations of state with different smooth interpolation functions has only a modest effect on the predicted mass, radius, and tidal deformability of neutron stars, provided the matching occu...
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Toward a Unified Understanding of the Dense Matter Equation of State
A review of three Bayesian/computational frameworks for combining heavy-ion and astrophysical constraints on the dense-matter equation of state, plus a proposed unified integration workflow.
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Nuclear matter equation of state and astrophysics
A review of multimessenger constraints on the neutron-star equation of state, arguing composition remains undetermined and advocating a multidimensional EoS framework and the author-affiliated MUSES software.
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The equation of state for neutron stars
A textbook-style review of the neutron-star equation of state covering the models, experimental and observational constraints, and open questions, with no new result claimed or derived.
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