Beta Equilibrium under Neutron Star Merger Conditions

Alford, Mark; Haber, Alexander; Harris, Steven P.; Zhang, Ziyuan

doi:10.3390/universe7110399

Cited by 32 publications

(34 citation statements)

References 63 publications

(92 reference statements)

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“…As already mentioned in Section 1, this is because the relation between Y I and Y Q is a trivial shift only when net strangeness is zero, but not otherwise. See Reference [104] for a complete discussion of the chemically equilibrated case at finite temperature.…”

Section: Resultsmentioning

confidence: 99%

The Effect of Charge, Isospin, and Strangeness in the QCD Phase Diagram Critical End Point

et al. 2021

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In this work, we discuss the deconfinement phase transition to quark matter in hot/dense matter. We examine the effect that different charge fractions, isospin fractions, net strangeness, and chemical equilibrium with respect to leptons have on the position of the coexistence line between different phases. In particular, we investigate how different sets of conditions that describe matter in neutron stars and their mergers, or matter created in heavy-ion collisions affect the position of the critical end point, namely where the first-order phase transition becomes a crossover. We also present an introduction to the topic of critical points, including a review of recent advances concerning QCD critical points.

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Section: Resultsmentioning

confidence: 99%

The Effect of Charge, Isospin, and Strangeness in the QCD Phase Diagram Critical End Point

et al. 2021

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“…However, it is important to keep in mind that the assumptions will not be appropriate for much of the parameter space (temperature and density) explored in the binary neutron star merger/post-merger phase, and they completely exclude any neutrino effects. At finite temperatures, the true notion of beta equilibrium is more complex, and may require the addition of an isospin chemical potential in the definition of β (see [29,[34][35][36]). A complete model should account for the correct notion of equilibrium, but this will require the equation of state table to be extended to include all necessary information.…”

Section: Hydrodynamics Of a Reactive Systemmentioning

confidence: 99%

“…The information encoded in the reaction rate Γ e is now "stored" in γ. We can then make progress and compute γ from the equation of state tables provided in the compOSE database [33] only as long as we ignore finite temperature effects [34][35][36]. While the coefficient B can be introduced without reference to an expansion around equilibrium, this is not the case for A.…”

Section: Hydrodynamics Of a Reactive Systemmentioning

confidence: 99%

Formulating bulk viscosity for neutron star simulations

Celora,

Hawke,

Hammond

et al. 2022

Preprint

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In order to extract the precise physical information encoded in the gravitational and electromagnetic signals from powerful neutron-star merger events, we need to include as much of the relevant physics as possible in our numerical simulations. This presents a severe challenge, given that many of the involved parameters are poorly constrained. In this paper we focus on the role of nuclear reactions. Combining a theoretical discussion with an analysis connecting to state-ofthe-art simulations, we outline multiple arguments that lead to a reactive system being described in terms of a bulk viscosity. The results demonstrate that in order to properly account for nuclear reactions, future simulations must be able to handle different regimes where rather different assumptions/approximations are appropriate. We also touch upon the link to models based on the large-eddy-strategy required to capture turbulence.

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“…On the other hand, the proton fraction inside the betaequilibrated matter also determines whether a protoneutron star will go through a cooling epoch via neutrino emmission through the direct Urca (DU) process n → p + e + νe , which is expected to occur if the proton fraction reaches a critical value, γ p > x DU , the so-called DU-threshold [39,40]. As the DU process allows for an enhanced cooling rate of NS, whether it takes place or not in the hot core of proto-neutron stars or during the merge of binary NS systems [41] would determine the proton fraction (hence, the symmetry energy) of matter at ultra-high densities. However, it is not clear whether such enhanced cooling actually takes place, although there is recent evidence that supports it [42].…”

Section: Particle Fractions Of Npeµ Matter In β-Equilibriummentioning

confidence: 99%

Quantum Skyrmion crystals and the symmetry energy of dense matter

Adam¹,

Martín-Caro²,

Huidobro³

et al. 2022

Preprint

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The canonical quantization method for collective coordinates in crystalline configurations of the generalized Skyrme model is applied in order to find the quantum ground state of Skyrmion crystals and study the quantum corrections to the binding energy resulting from the isospin degrees of freedom. This leads to a consistent description of asymmetric nuclear matter within the Skyrme framework and allows us to compute the symmetry energy of the Skyrmionic crystal as a function of the baryon density, and to compare with recent observational constraints. CONTENTS I. Introduction 1 II. Generalized Skyrme model and classical crystals 2 A. The model 2 B. The classical crystal of Skyrmions 3 C. The Skyrme crystal EoS for symmetric nuclear matter 3 III. Quantization of the Skyrme crystal 4 A. The internal symmetry of Skyrme crystals and the isospin group 4 B. Quantum isospin states and Hilbert space 5 C. Isospin correction to the energy per baryon 7 IV. Quantum skyrmion crystals and the symmetry energy of npe(µ) matter 9 A. The electric charge density of pure Skyrmion matter 9 B. The symmetry energy 10 C. Particle fractions of npeµ matter in β-equilibrium 11 V. Conclusions 12 Acknowledgments 13 A. Calculation of matrix elements 13 B. Isospin inertia tensor of Skyrme crystals 14 References 15

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Beta Equilibrium under Neutron Star Merger Conditions

Cited by 32 publications

References 63 publications

The Effect of Charge, Isospin, and Strangeness in the QCD Phase Diagram Critical End Point

The Effect of Charge, Isospin, and Strangeness in the QCD Phase Diagram Critical End Point

Formulating bulk viscosity for neutron star simulations

Quantum Skyrmion crystals and the symmetry energy of dense matter

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