Analytical representations of unified equations of state of neutron-star matter
By A. Potekhin, A. Fantina, N. Chamel, J. Pearson, S. Goriely. 2004
299 citations recorded by the source corpus.
Analytical representations are derived for two equations of state (EOSs) of neutron-star matter: FPS and SLy. Each of these EOSs is unified, that is, it describes the crust and the core of a neutron star using the same physical model. Two versions of the EOS parametrization are considered. In the first one, pressure and mass density are given as functions of the baryon density. In the second version, pressure, mass density, and baryon density are given as functions of the pseudo-enthalpy, which makes this representation particularly useful for 2-D calculations of stationary rotating configurations of neutron stars.
Subfields: Astronomy and Astrophysics, Geophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/26296c4f54045192c812c05ddd0a4a2d5a0d6de2
How researchers see this paper
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In Astronomy and Astrophysics
- Diego Rubiera-García
- José A. Pons
- D. Page
- G. Fiorella Burgio
- Aneta Wojnar
- A. Potekhin
- Marc A. Baldo
- M. Centelles
In Geophysics
- G. Fiorella Burgio
- José A. Pons
- D. Page
- Marc A. Baldo
- Diego Rubiera-García
- G. Olmo
- Aneta Wojnar
- A. Potekhin
In Nuclear and High Energy Physics
- G. Fiorella Burgio
- Diego Rubiera-García
- Aneta Wojnar
- José A. Pons
- D. Page
- Marc A. Baldo
- M. Centelles
- B. Sharma
Citations in the corpus
- Unified equation of state for neutron stars on a microscopic basis (2015, methodology): “…2010) as a representative example of contemporary EoS for the complete NS structure, and a comparison with the other EoSs of the BSk family (Chamel et al. 2011; Pearson et al. 2012; Fantina et al. 2013; Potekhin et al. 2013) and the RMF family (Shen et al. 2011b,a) shall be left for future study.”
- Neutron Stars—Cooling and Transport (2015, methodology): “The latter parameter has been fitted as function of density for modern BSk models of nuclear matter (Potekhin et al. 2013) and for some other models (Appendix B in Haensel et al. 2007).”
- Stellar structure models in modified theories of gravity: Lessons and challenges (2019, methodology): “Choosing EOS for the radial pressure to be FPS, SLy, BSk21 in terms of their analytical representations [203, 210], for values α = −5×1010cm2 and α = −20×1010cm2, numerical resolution of the TOV equations yields a slight increase of M⋆ up to ∼ 5% for all these scenarios, with also slight decreases o”