Maximal Mass Neutron Star as a Key to Superdense Matter Physics
arXiv:2310.16847 · doi:10.1134/S1063773723100055
Abstract
We propose a universal approximation of the equation of state of superdense matter in neutron star (NS) interiors. It contains only two parameters, the pressure and the density at the center of the maximally massive neutron star. We demonstrate the validity of this approximation for a wide range of different types of equations of state, including both baryonic and hybrid models. Combined with recently discovered correlations of internal (density, pressure, and speed of sound at the center) and external (mass, radius) properties of a maximally massive neutron star, this approximation turns out to be an effective tool for determining the equation of state of superdense matter using astrophysical observations.
13 pages, 5 figures, 2 tables. Various improvements according to feedback and proof reading. Data for the JJ EoSs is corrected w.r.t. the journal version
References in corpus (10)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Multi-messenger Observations of a Binary Neutron Star Merger
- Constraints on a phenomenologically parameterized neutron-star equation of state
- Spectral Representations of Neutron-Star Equations of State
- Cooling rates of neutron stars and the young neutron star in the Cassiopeia A supernova remnant
- Thermal emission of neutron stars with internal heaters
- Bulk viscosity in neutron stars with hyperon cores
- Universal properties of maximum-mass neutron stars: a new tool to explore superdense matter
- Core States of Neutron Stars from Anatomizing their Scaled Structure Equations
Cited by in corpus (5)
- Novel Scalings of Neutron Star Properties from Analyzing Dimensionless Tolman--Oppenheimer--Volkoff Equations
- Towards constraining QCD phase transitions in neutron star interiors: Bayesian Inference with TOV linear response analysis
- Strong Gravity Extruding Peaks in Speed of Sound Profiles of Massive Neutron Stars
- Correlations between the Neutron Star Mass-Radius Relation and the Equation of State of Dense Matter
- New Insights into Supradense Matter from Dissecting Scaled Stellar Structure Equations