Neutron star equation of state: identifying hadronic matter characteristics
arXiv:2307.05086 · doi:10.1201/9781003306580-5
Abstract
The general behavior of the nuclear equation of state (EOS), relevant for the description of neutron stars (NS), is studied within a relativistic mean field description of nuclear matter. Different formulations, both with density dependent couplings and with non-linear mesonic terms, are considered and their predictions compared and discussed. A special attention is drawn to the effect on the neutron star properties of the inclusion of exotic degrees of freedom as hyperons. Properties such as the speed of sound, the trace anomaly, the proton fraction and the onset of direct Urca processes inside neutron stars are discussed. The knowledge of the general behavior of the hadronic equation of state and the implication it has on the neutron star properties will allow to identify signatures of a deconfinement phase transition discussed in other studies.
arXiv comment16 pages, 11 figures
References in corpus (65)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- GW170817: Measurements of Neutron Star Radii and Equation of State
- 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
- X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue
- Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar
- Tidal Love numbers of neutron stars
- Properties of the binary neutron star merger GW170817
- Refined Mass and Geometric Measurements of the High-Mass PSR J0740+6620
- Composition and thermodynamics of nuclear matter with light clusters
- The Equation of State from Observed Masses and Radii of Neutron Stars
- Neutron Star Structure and the Neutron Radius of 208Pb
- Neutron Star Cooling
- Neutron-Rich Nuclei in Heaven and Earth
- Evidence for quark-matter cores in massive neutron stars
- Neutrino Emission from Neutron Stars
- Cold Quark Matter
- Relativistic Mean-Field Hadronic Models under Nuclear Matter Constraints
- Relativistic Mean-Field Theory and the High-Density Nuclear Equation of State
- Strangeness in nuclear physics
- The Neutron Star Mass-Radius Relation and the Equation of State of Dense Matter
- Astrophysical Measurement of the Equation of State of Neutron Star Matter
- Chiral interactions up to next-to-next-to-next-to-leading order and nuclear saturation
- Neutron star radii and crusts: uncertainties and unified equations of state
- Hyperons and massive neutron stars: the role of hyperon potentials
- Asymmetric nuclear matter:the role of the isovector scalar channel
- The equation of state for dense nucleonic matter from a metamodeling. I. Foundational aspects
- On the Sound Speed in Neutron Stars
- Spectral Representations of Neutron-Star Equations of State
- Non-parametric inference of the neutron star equation of state from gravitational wave observations
- Nonparametric Inference of Neutron Star Composition, Equation of State, and Maximum Mass with GW170817
- How perturbative QCD constrains the Equation of State at Neutron-Star densities
- The equation of state for dense nucleonic matter from a meta-modeling. II. Predictions for neutron stars properties
- Trace anomaly as signature of conformality in neutron stars
- Quantifying uncertainties and correlations in the nuclear-matter equation of state
- Dense matter with eXTP
- (No) neutron star maximum mass constraint from hypernuclei
- Mapping neutron star data to the equation of state using the deep neural network
- Neutron star properties and the symmetry energy
- Combining Electromagnetic and Gravitational-Wave Constraints on Neutron-Star Masses and Radii
- A Detailed Examination of Astrophysical Constraints on the Symmetry Energy and the Neutron Skin of Pb with Minimal Modeling Assumptions
- Bayesian Inference of the Symmetry Energy of Super-Dense Neutron-Rich Matter from Future Radius Measurements of Massive Neutron Stars
- Relativistic description of dense matter equation of state and compatibility with neutron star observables: a Bayesian approach
- Neutron stars with hyperon cores: stellar radii and EOS near nuclear density
- Methodology study of machine learning for the neutron star equation of state
- Relativistic hypernuclear compact stars with calibrated equations of state
- Hyperonic stars and the symmetry energy
- Perturbative QCD and the Neutron Star Equation of State
- Statistical theory of thermal evolution of neutron stars - II. Limitations on direct Urca threshold
- Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states
- Unveiling the nuclear matter EoS from neutron star properties: a supervised machine learning approach
- Thermal evolution of relativistic hyperonic compact stars with calibrated equations of state
- Large and massive neutron stars: Implications for the sound speed in dense QCD
- Bayesian Inference of the Dense Matter Equation of State built upon Covariant Density Functionals
- Bayesian reconstruction of nuclear matter parameters from the equation of state of neutron star matter
- Empirical constraints on the high-density equation of state from multi-messenger observables
- Constraints on high density equation of state from maximum neutron star mass
- Neutron stars: from the inner crust to the core with the (Extended) Nambu-Jona-Lasinio model
- Determination of the symmetry energy from the neutron star equation of state
- How far is normal nuclear matter from the chiral symmetry restoration?
- Nonparametric model for the equations of state of neutron star from deep neural network
- Symmetry energy and neutron star properties in the saturated Nambu-Jona-Lasinio model
- Constraining a relativistic mean field model using neutron star mass-radius measurements I: Nucleonic models