Probing crustal structures from neutron star compactness
arXiv:1706.04736 · doi:10.1093/mnras/stx1510
Abstract
With various sets of the parameters that characterize the equation of state (EOS) of nuclear matter, we systematically examine the thickness of a neutron star crust and of the pasta phases contained therein. Then, with respect to the thickness of the phase of spherical nuclei, the thickness of the cylindrical phase, and the crust thickness, we successfully derive fitting formulas that express the ratio of each thickness to the star's radius as a function of the star's compactness, the incompressibility of symmetric nuclear matter, and the density dependence of the symmetry energy. In particular, we find that the thickness of the phase of spherical nuclei has such a strong dependence on the stellar compactness as the crust thickness, but both of them show a much weaker dependence on the EOS parameters. Thus, via determination of the compactness, the thickness of the phase of spherical nuclei as well as the crust thickness can be constrained reasonably, even if the EOS parameters remain to be well-determined.
accepted for publication in MNRAS
References in corpus (28)
- Constraints on the symmetry energy and neutron skins from experiments and theory
- A giant, periodic flare from the soft gamma repeater SGR1900+14
- Incompressibility in finite nuclei and nuclear matter
- Disordered nuclear pasta, magnetic field decay, and crust cooling in neutron stars
- A highly resistive layer within the crust of X-ray pulsars limits their spin periods
- The symmetry energy at subnuclear densities and nuclei in neutron star crusts
- Structure of cold nuclear matter at subnuclear densities by Quantum Molecular Dynamics
- Probing the Equation of State of Nuclear Matter via Neutron Star Asteroseismology
- Constraints on Neutron Star Crusts From Oscillations in Giant Flares
- Upper limits on the observational effects of nuclear pasta in neutron stars
- Neutron star oscillations and QPOs during magnetar flares
- Effect of superfluidity on neutron star crustal oscillations
- Saturation of nuclear matter and radii of unstable nuclei
- Possible Constraints on the Density Dependence of the Nuclear Symmetry Energy from Quasiperiodic Oscillations in Soft Gamma Repeaters
- Pasta Nucleosynthesis: Molecular dynamics simulations of nuclear statistical equilibrium
- Spin-Down of Neutron Stars and Compositional Transitions in the Cold Crustal Matter
- Possible identifications of newly observed magnetar quasi-periodic oscillations as crustal shear modes
- Topological characterization of neutron star crusts
- Constraints on the symmetry energy from observational probes of the neutron star crust
- Constraints on Pasta Structure of Neutron Stars from Oscillations in Giant Flares
- Probing nuclear bubble structure via neutron star asteroseismology
- The cooling of the Cassiopeia A neutron star as a probe of the nuclear symmetry energy and nuclear pasta
- Nuclear Pasta Matter for Different Proton Fractions
- Quasi-periodic oscillations in superfluid, relativistic magnetars with nuclear pasta phases
- Empirical formula of crustal torsional oscillations
- Electron screening effects on crustal torsional oscillations
- Symmetry energy, unstable nuclei, and neutron star crusts
- Formation scenarios and mass-radius relation for neutron stars
Cited by in corpus (21)
- From hadrons to quarks in neutron stars: a review
- Insights on Skyrme parameters from GW170817
- Constraints on the nuclear equation of state and the neutron star structure from crustal torsional oscillations
- Astrophysical implications of double-layer torsional oscillations in a neutron star crust as a lasagna sandwich
- Gravitational wave asteroseismology for low-mass neutron stars
- Neutron star mass-radius constraints using the high-frequency QPOs of GRB 200415A
- Magnetar QPOs and neutron star crust elasticity
- Effects of the equation of state on the core-crust interface of slowly rotating neutron stars
- Constraints on Skyrme Equations of State from Doubly Magic Nuclei, Ab-Initio Calculations of Low-Density Neutron Matter, and Neutron Stars
- Shear and interface modes in neutron stars with pasta structures
- Shear oscillations in neutron stars and the nuclear symmetry energy
- Roles of crust and core in the tidal deformability of neutron stars
- Crust Cooling Models are Insensitive to the Crust-Core Transition Pressure for Realistic Equations of State
- Effects of finite sizes of atomic nuclei on shear modulus and torsional oscillations in neutron stars
- Zeeman splitting of torsional oscillation frequencies of magnetars
- Nuclear masses and the equation of state of nuclear matter
- Selfsimilarity relations for torsional oscillations of neutron stars
- Powerful flares and magneto-elastic oscillations of magnetars
- Impact of the relativistic Cowling approximation on shear and interface modes of neutron stars
- Estimation of neutron star mass and radius of FRB 20240114A by identification of crustal oscillations
- Zeeman effect in oscillations of magnetars with toroidal magnetic fields