Reconciling Nuclear and Astrophysical Constraints
arXiv:1503.07785 · doi:10.1103/PhysRevC.92.012801
Abstract
In view of new constraints put forth by recent observations and measurements in the realm of astrophysics and nuclear physics, we update the non-linear realization of the sigma model as to reflect such constraints. By doing this, we obtain new equations of state that may be used to describe neutron stars. Such equations of state are obtained by investigating different ways by which the vector mesons self-interact. Furthermore, we also investigate the role played by the delta mesons in the model. As a result, we are able to develop equations of state that are in better agreement with data, such as nuclear compressibility and slope of the symmetry energy at saturation, star masses, radii, and cooling profiles.
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Cited by in corpus (7)
- Equation of State for Nucleonic and Hyperonic Neutron Stars with Mass and Radius Constraints
- Equations of state for hot neutron stars -- II. The role of exotic particle degrees of freedom
- The application of the Quark-Hadron Chiral Parity-Doublet Model to neutron star matter
- The internal composition of proto-neutron stars under strong magnetic fields
- Effect of isovector scalar meson on equation of state of dense matter within relativistic mean field model
- Universal relations for the Keplerian sequence of rotating neutron stars
- Universal Relations for rapidly rotating neutron stars using supervised machine-learning techniques