TL;DR
This paper discusses how recent neutron star mass measurements constrain the equation of state (EOS) of neutron star matter, emphasizing model-independent limits, the importance of non-perturbative quark matter treatments, and the potential of mass-radius data to determine the EOS.
Contribution
It introduces model-independent upper limits on neutron star properties based on maximum mass and highlights the need for non-perturbative quark matter models in neutron star studies.
Findings
Upper limits on thermodynamic properties derived from causality and maximum mass.
Non-perturbative treatments are essential for understanding quark matter in neutron stars.
Mass and radius measurements can help invert stellar structure equations to constrain the EOS.
Abstract
Implications of recently well-measured neutron star masses, particularly near and above 2 solar masses, for the equation of state (EOS) of neutron star matter are highlighted. Model-independent upper limits to thermodynamic properties in neutron stars, which only depend on the neutron star maximum mass, established from causality considerations are presented. The need for non-perturbative treatments of quark matter in neutron stars is stressed through studies of self-bound quark matter stars, and of nucleon-quark hybrid stars. The extent to which several well-measured masses and radii of individual neutron stars can establish a model-independent EOS through an inversion of the stellar structure equations is briefly discussed.
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.