Isospin asymmetric nuclear matter and properties of axisymmetric neutron stars

Abstract

Pure hadronic compact stars, above a limiting value ($\approx$1.6 M${}_{\odot }$) of their gravitational masses, to which predictions of most of other equations of state (EoSs) are restricted, can be reached from the equation of state (EoS) obtained using DDM3Y effective interaction. This effective interaction is found to be quite successful in providing unified description of elastic and inelastic scattering, various radioactivities and nuclear matter properties. We present a systematic study of the properties of pure hadronic compact stars. The $\beta$-equilibrated neutron star matter using this EoS with a thin crust is able to describe highly-massive compact stars, such as PSR B1516+02B with a mass M=1.94${}_{-0.19}^{+0.17}$ M${}_{\odot }$ and PSR J0751+1807 with a mass M=2.1$\pm$0.2 M${}_{\odot }$ to a 1$\sigma$ confidence level.

arXiv comment5 pages, 4 figures

References in corpus (36)

• Determination of the Equation of State of Dense Matter
• Neutron Star Observations: Prognosis for Equation of State Constraints
• Recent Progress and New Challenges in Isospin Physics with Heavy-Ion Reactions
• A Radio Pulsar Spinning at 716 Hz
• Rotating Stars in Relativity
• Comparing Models of Rapidly Rotating Relativistic Stars Constructed by Two Numerical Methods
• Determination of the stiffness of the nuclear symmetry energy from isospin diffusion
• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Phases of dense matter in neutron stars
• EXO 0748-676 Rules out Soft Equations of State for Neutron Star Matter
• Circumstantial evidence for a soft nuclear symmetry energy at supra-saturation densities
• A 2.1 Solar Mass Pulsar Measured by Relativistic Orbital Decay
• Eight New Millisecond Pulsars in NGC 6440 and NGC 6441
• Alpha decay half-lives of new superheavy elements
• Further Constraints on Thermal Quiescent X-ray Emission from SAX J1808.4-3658
• Predictions of Alpha Decay Half lives of Heavy and Superheavy Elements
• Cooling of the quasi-persistent neutron star X-ray transients KS 1731-260 and MXB 1659-29
• A Massive Neutron Star in the Globular Cluster M5
• Super-soft symmetry energy encountering non-Newtonian gravity in neutron stars
• Search for long lived heaviest nuclei beyond the valley of stability
• Folding model analysis of proton radioactivity of spherical proton emitters
• Role of effective interaction in nuclear disintegration processes
• R-modes of accreting hyperon stars as persistent sources of gravitational waves
• Deconfinement Phase Transition in Compact Stars : Maxwell vs. Gibbs Construction of the Mixed Phase
• Nuclear Half-Lives for Alpha Radioactivity of Elements with 100 $\le$ Z $\le$ 130
• Alpha decay chains from element 113
• Catastrophic rearrangement of a compact star due to the quark core formation
• The Cooling Neutron Star in 3C 58
• Nuclear equation of state at high baryonic density and compact star constraints
• Isospin dependent properties of asymmetric nuclear matter
• Spontaneous heavy cluster emission rates using microscopic potentials
• Spin polarised nuclear matter and its application to neutron stars
• Folding model analysis of proton scattering from mirror nuclei ${}^{18}$Ne and ${}^{18}$O
• Rotating Twin Stars and Signature of Quark-Hadron Phase Transition
• Isobaric incompressibility of the isospin asymmetric nuclear matter
• Folding model analysis of proton scattering from ${}^{18,20,22}$O nuclei

Cited by in corpus (8)

• Neutron stars with small radii -- the role of delta resonances
• Stability of the $\beta$-equilibrated dense matter and core-crust transition in neutron stars
• Gravitational waves from isolated neutron stars: mass dependence of r-mode instability
• Core-crust transition and crustal fraction of moment of inertia in neutron stars
• From nuclear reactions to compact stars: a unified approach
• Rapidly rotating axisymmetric neutron stars with quark cores
• Properties of glitching pulsars in the Skyrme-Hartree-Fock framework
• Effective interaction: From nuclear reactions to neutron stars