Neutron Star Inner Crust at Finite Temperatures: A Comparison Between Compressible Liquid Drop and Extended Thomas-Fermi Approaches
arXiv:2505.19984 · doi:10.3390/universe11060172
Abstract
We investigate the effects of temperature on the properties of the inner crust of a non-accreting neutron star. To this aim, we employ two different treatments: the compressible liquid drop model (CLDM) and the temperature-dependent extended Thomas-Fermi (TETF) method. Our systematic comparison shows an agreement between the two methods on their predictions for the crust thermodynamic properties. We find that the CLDM description can also reproduce reasonably well the TETF composition especially if the surface energy is optimized on the ETF calculation. However, the neglect of neutron skin in CLDM leads to an overestimation of the proton radii.
References in corpus (40)
- Equations of state for supernovae and compact stars
- Neutron Star Cooling
- Composition and Structure of Protoneutron Stars
- Core-collapse supernova equations of state based on neutron star observations
- Physics of Neutron Star Crusts
- Statistical Model for a Complete Supernova Equation of State
- Evolution of Protoneutron Stars
- Neutron Stars and the Nuclear Equation of State
- The equation of state for dense nucleonic matter from a metamodeling. I. Foundational aspects
- Relativistic Equation of State for Core-Collapse Supernova Simulations
- Thermal Relaxation in Young Neutron Stars
- Further explorations of Skyrme-Hartree-Fock-Bogoliubov mass formulas. XI: Stabilizing neutron stars against a ferromagnetic collapse
- Nuclear equation of state for core-collapse supernova simulations with realistic nuclear forces
- Nuclear pasta structures and the charge screening effect
- A New Open-Source Nuclear Equation of State Framework based on the Liquid-Drop Model with Skyrme Interaction
- Isospin-dependent clusterization of Neutron-Star Matter
- A survey of the parameter space of the compressible liquid drop model as applied to the neutron star inner crust
- Semi-classical equation of state and specific heats for neutron-star inner crust with proton shell corrections
- On the validity of the Wigner-Seitz approximation in neutron star crust
- Evolution of a proto-neutron star with a nuclear many-body equation of state: Neutrino luminosity and gravitational wave frequencies
- Neutrino transport in general relativistic neutron star merger simulations
- New equations of state based on the liquid drop model of heavy nuclei and quantum approach to light nuclei for core-collapse supernova simulations
- Neutron star crusts from mean field models constrained by chiral effective field theory
- Modelling neutron star mountains
- Proto-neutron star evolution with improved charged-current neutrino-nucleon interactions
- Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. II. Pasta phases in semi-classical approximation
- Beta equilibrium under neutron star merger conditions
- Uncertainties in the pasta-phase properties of catalysed neutron stars
- Crystallization of the inner crust of a neutron star and the influence of shell effects
- Nuclear Statistical Equilibrium Equation of State for Core Collapse
- Pasta properties of the neutron star within effective relativistic mean-field model
- Comparison between the Thomas-Fermi and Hartree-Fock-Bogoliubov Methods in the Inner Crust of a Neutron Star: The Role of Pairing Correlations
- Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. IV. Role of the symmetry energy in pasta phases
- Unified equations of state for cold nonaccreting neutron stars with Brussels-Montreal functionals. V. Improved parametrization of the nucleon density distributions
- The proto-neutron star inner crust in the liquid phase
- The proto-neutron star inner crust in a multi-component plasma approach
- Parametrization of the surface energy in the ETF approximation
- Time-dependent nuclear energy-density functional theory toolkit for neutron star crust: Dynamics of a nucleus in a neutron superfluid
- Impact of Hot Inner Crust on Compact Stars at Finite Temperature
- Role of neutron pairing with density-gradient dependence in the semi-microscopic treatment of the inner crust of neutron stars