The neutron star inner crust: an empirical essay

Abstract

In this work we study how the small contribution of the inner crust to the total equation of state (EoS) of a neutron star affects its mass-radius relation, focusing on the canonical mass of 1.4$M_{\odot }$. We build empirical EoS of the kind - $p=K{\epsilon }^{\gamma }+b$ - in the range of 0.003 fm${}^{-3}<n<$0.08 fm${}^{-3}$ and also calculate the speed of sound in this region. We see that different behaviours of the speed of sound can affect the radius of the canonical star by more than 1.1 km. This result can help us understand extreme results as GW170817, where some studies indicate that the radius of the canonical star cannot exceed 11.9 km.

arXiv commentletter, Published version

References in corpus (35)

• A Massive Pulsar in a Compact Relativistic Binary
• PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
• A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
• Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar
• Determination of the Equation of State of Dense Matter
• Equations of state for supernovae and compact stars
• Constraints on the symmetry energy and neutron skins from experiments and theory
• Evidence for quark-matter cores in massive neutron stars
• Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
• Neutron skins and neutron stars in the multi-messenger era
• Stringent constraints on neutron-star radii from multimessenger observations and nuclear theory
• Constraints on neutron star radii based on chiral effective field theory interactions
• Hyperons and massive neutron stars: vector repulsion and SU(3) symmetry
• Asymmetric nuclear matter:the role of the isovector scalar channel
• Constraints on the Symmetry Energy Using the Mass-Radius Relation of Neutron Stars
• Neutron Star Masses and Radii from Quiescent Low-Mass X-ray Binaries
• Discovery of absorption features in the X-ray spectrum of an isolated neutron star
• Proto-Neutron and Neutron Stars in a Chiral SU(3) Model
• Magnetic Hydrogen Atmosphere Models and the Neutron Star RX J1856.5-3754
• Inner edge of neutron-star crust with SLy effective nucleon-nucleon interactions
• The equation of state of neutron matter, symmetry energy, and neutron star structure
• Hypernuclear matter in a complete SU(3) symmetry group
• Neutron star properties and the symmetry energy
• The pasta phase within density dependent hadronic models
• Strong correlations of neutron star radii with the slopes of nuclear matter incompressibility and symmetry energy at saturation
• Speed of sound constraints from tidal deformability of neutron stars
• Neutron Stars with Hyperons subject to Strong Magnetic Field
• Broken SU(6) symmetry and massive hybrid stars
• Neutron star collapse and gravitational waves with a non-convex equation of state
• Role of vector channel in different classes of (non) magnetized neutron stars
• Effect of Inner Crust EoS on Neutron star properties
• Hyperon threshold and stellar radii
• Effects of the Symmetry Energy and its Slope on Neutron Star Properties
• The importance of strange mesons in neutron star properties
• Core-crust transition pressure for relativistic slowly rotating neutron stars

Cited by in corpus (10)

• Relativistic description of dense matter equation of state and compatibility with neutron star observables: a Bayesian approach
• Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions
• A Neutron Star is born
• Quark Models and Radial Oscillations: Decoding the HESS J1731-347 Compact Object's Equation of State
• Delta baryons in neutron stars
• Hyperonic neutron stars: reconciliation between nuclear properties and NICER and LIGO/VIRGO results
• Radial Oscillations in Neutron Stars with Delta Baryons
• Oscillatory properties of strange quark stars described by the vector MIT bag model
• Macroscopic properties of the XTE J1814-338 as a dark matter admixed strange star
• Effects of the symmetry energy slope on magnetized neutron stars