Constraining neutron star matter from the slope of the mass-radius curves

Abstract

We analyse the implications of information about local derivatives from the mass-radius diagram in neutron star matter. It is expected that the next generation of gravitational wave and electromagnetic detectors will allow the determination of the neutron star radius and mass with a small uncertainty. Observations of neutron stars clustered around a given neutron star mass allow the estimation of local derivatives in the $M(R)$ diagram, which can be used to constrain neutron star properties. From a model-independent description of the neutron star equation of state, it is shown that a $M(R)$ curve with a negative slope at 1.4$M_{\odot }$ predicts a $2M_{\odot }$ neutron star radius below 12 km. Furthermore, a maximum mass below 2.3$M_{\odot }$ is obtained if the $M(R)$ slope is negative in the whole range of masses above $1M_{\odot }$, and a maximum mass above 2.4$M_{\odot }$ requires the $M(R)$ slope to be positive in some range of masses. Constraints on the mass-radius curve of neutron stars will place strong constraints on microscopic models.

arXiv comment10 pages, 11 figures, title changed, published version

References in corpus (44)

• 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
• A New Parameterization for the Lagrangian Density of Relativistic Mean Field Theory
• A unified equation of state of dense matter and neutron star structure
• Properties of the binary neutron star merger GW170817
• A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy
• Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral
• Gravitational-wave constraints on the neutron-star-matter Equation of State
• Composition and thermodynamics of nuclear matter with light clusters
• Neutron Star Structure and the Neutron Radius of 208Pb
• Constraints on a phenomenologically parameterized neutron-star equation of state
• Equation of state and neutron star properties constrained by nuclear physics and observation
• Evidence for quark-matter cores in massive neutron stars
• The Neutron Star Mass-Radius Relation and the Equation of State of Dense Matter
• Relativistic effective interaction for nuclei, giant resonances, and neutron stars
• Nonparametric constraints on neutron star matter with existing and upcoming gravitational wave and pulsar observations
• Neutron star radii and crusts: uncertainties and unified equations of state
• Quarkyonic Matter and Neutron Stars
• The enhanced X-ray Timing and Polarimetry mission - eXTP
• Building relativistic mean field models for finite nuclei and neutron stars
• Multimessenger Parameter Estimation of GW170817
• On the Sound Speed in Neutron Stars
• GW190814: Impact of a 2.6 solar mass neutron star on nucleonic equations of state
• Dense Nuclear Matter Equation of State from Heavy-Ion Collisions
• Multimessenger constraints for ultra-dense matter
• Trace anomaly as signature of conformality in neutron stars
• Dense matter with eXTP
• Quarkyonic Matter Equation of State in Beta-Equilibrium
• Mapping neutron star data to the equation of state using the deep neural network
• The Equation of State for the Nucleonic and Hyperonic Core of Neutron Stars
• New equations of state constrained by nuclear physics, observations, and QCD calculations of high-density nuclear matter
• The Vlasov formalism for extended relativistic mean field models: the crust-core transition and the stellar matter equation of state
• Theoretical and Experimental Constraints for the Equation of State of Dense and Hot Matter
• Relativistic description of dense matter equation of state and compatibility with neutron star observables: a Bayesian approach
• From Neutron Star Observables to the Equation of State. II. Bayesian Inference of Equation of State Pressures
• Equation-of-state insensitive relations after GW170817
• Hyperons in hot dense matter: what do the constraints tell us for equation of state?
• Quark matter in light neutron stars
• Constraints on high density equation of state from maximum neutron star mass
• Constraining Nuclear Symmetry Energy with Multi-messenger Resonant Shattering Flares
• Structure of Quark Star: A Comparative Analysis of Bayesian Inference and Neural Network Based Modeling
• From NS observations to nuclear matter properties: a machine learning approach
• Neutron star equation of state: identifying hadronic matter characteristics

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• On the maximum compactness of neutron stars
• Unraveling Trace Anomaly of Supradense Matter via Neutron Star Compactness Scaling
• Bayesian Inference of Hybrid Star Properties from Future High-Precision Measurements of Their Radii
• New Insights into Supradense Matter from Dissecting Scaled Stellar Structure Equations
• Effective Field Theories for Neutron Stars Physics
• Is The Trace Anomaly at its Minimum Value at Neutron Star Centers?
• Learning about neutron star composition from the slope of the mass-radius diagram
• Bayesian Inference of fine-features of dense matter EOS from future high-precision data of neutron star radii