Effects of dilute neutron matter on the neutron star crust equation of state
arXiv:2401.13590 · doi:10.1140/epja/s10050-024-01309-3
Abstract
We develop a compressible liquid-drop model to describe the crust of neutron stars for which the role of the nuclear clusters, the neutron gas, and the electrons are clearly identified. The novelty relies on the contribution of the neutron gas, which is qualitatively adjusted to reproduce 'ab initio' predictions in dilute neutron matter. We relate the properties of dilute neutron matter to the ones of neutron stars crust and we compare the mean-field approximation to an improved approach that better describes dilute neutron matter. The latter is quite sensitive to the unitary limit, a universal feature of Fermi systems having a large value of the scattering length and a small interaction range. While the impact of the accurate description of dilute neutron matter is important in uniform matter (up to 30\% corrections with respect to a mean-field calculations), we find a reduction of this impact in the context of the crust of neutron stars due to the additional matter components (nuclear clusters and electrons). In agreement with our previous works, dilute neutron matter is however a necessary ingredient for accurate predictions of the properties of the crust of neutron stars.
References in corpus (36)
- Revealing the Superfluid Lambda Transition in the Universal Thermodynamics of a Unitary Fermi Gas
- Large momentum part of fermions with large scattering length
- Superfluid Fermi Gases with Large Scattering Length
- The Equation of State of a Low-Temperature Fermi Gas with Tunable Interactions
- How well do we know the neutron-matter equation of state at the densities inside neutron stars? A Bayesian approach with correlated uncertainties
- Influence of Induced Interactions on the Superfluid Transition in Dilute Fermi Gases
- Low-density neutron matter
- Strongly paired fermions: Cold atoms and neutron matter
- Universal behavior of pair correlations in a strongly interacting Fermi gas
- Asymmetric nuclear matter based on chiral two- and three-nucleon interactions
- The equation of state for dense nucleonic matter from a meta-modeling. II. Predictions for neutron stars properties
- Spatial structure of neutron Cooper pair in low density uniform matter
- Neutron Matter from Low to High Density
- Screening Effects in Superfluid Nuclear and Neutron Matter within Brueckner Theory
- BCS-BEC crossover of neutron pairs in symmetric and asymmetric nuclear matter
- Low-energy collective excitations in the neutron star inner crust
- Constraints on the nuclear symmetry energy from asymmetric-matter calculations with chiral NN and 3N interactions
- Neutron matter at finite temperature based on chiral effective field theory interactions
- Ground-state thermodynamic quantities of homogeneous spin- fermions from the BCS region to the unitarity limit
- Glitch rises as a test for rapid superfluid coupling in neutron stars
- Superfluid Fermi atomic gas as a quantum simulator for the study of neutron-star equation of state
- Pairing in exotic neutron rich nuclei around the drip line and in the crust of neutron stars
- Densities and energies of nuclei in dilute matter
- Pair correlations of an expanding superfluid Fermi gas
- Strong-coupling corrections to ground-state properties of a superfluid Fermi gas
- Nuclear Superfluidity and Cooling Time of Neutron-Star Crust
- A superfluid perspective on neutron star dynamics
- The S pairing gap in neutron matter
- From resonantly interacting fermions with effective range to neutron matter
- Cold Atom Quantum Simulator for Dilute Neutron Matter
- Confronting a set of Skyrme and predictions for the crust of neutron stars
- Repeating Fast Radio Bursts with High Burst Rates by Plate Collisions in Neutron Star Crusts
- Equation of state of superfluid neutron matter with low-momentum interactions
- Pairing correlations of cold fermionic gases at overflow from a narrow to a wide harmonic trap
- Finite-temperature infinite matter with effective-field-theory-inspired energy-density functionals
- Effect of the equation of state for dilute neutron matter on the composition of the inner crust of neutron stars