The equation of state of dense matter : from nuclear collisions to neutron stars

@article{Burgio2008TheEO,
  title={The equation of state of dense matter : from nuclear collisions to neutron stars},
  author={Fiorella Burgio},
  journal={Journal of Physics G},
  year={2008},
  volume={35},
  pages={014048}
}
  • F. Burgio
  • Published 27 July 2007
  • Physics
  • Journal of Physics G
The equation of state (EoS) of dense matter represents a central issue in the study of compact astrophysical objects and heavy ion reactions at intermediate and relativistic energies. We have derived a nuclear EoS with nucleons and hyperons within the Brueckner-Hartree-Fock approach, and joined it with quark matter EoS. For that, we have employed the MIT bag model, as well as the Nambu-Jona-Lasinio and the color dielectric models, and found that the NS maximum masses are not larger than 1.7… 
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References

SHOWING 1-10 OF 61 REFERENCES
Determination of the Equation of State of Dense Matter
TLDR
This work analyzed the flow of matter to extract pressures in excess of 1034 pascals, the highest recorded under laboratory-controlled conditions, and ruled out strongly repulsive nuclear equations of state from relativistic mean field theory and weakly repulsive equation of state with phase transitions at densities less than three times that of stable nuclei.
Neutron star properties and the equation of state of neutron-rich matter
We calculate total masses and radii of neutron stars for pure neutron matter and nuclear matter in \ensuremath{\beta} equilibrium. We apply a relativistic nuclear matter equation of state derived
Hybrid stars with the color dielectric and the MIT bag models
We study the hadron-quark phase transition in the interior of neutron stars (NS). For the hadronic sector, we use a microscopic equation of state (EOS) involving nucleons and hyperons derived within
Evidence for a Soft Nuclear Equation-of-State from Kaon Production in Heavy-Ion Collisions.
TLDR
The ratio of the K+ meson excitation functions for Au+Au and C+C collisions increases with decreasing beam energy, which is expected for a soft nuclear equation-of-state.
EOS of Neutron-Rich Matter with a Microscopic Three-Body Force
The equation of state of neutron-rich matter is studied in the framework of the Brueckner-Bethe-Goldstone approach. In addition to the bare two-body force a microscopic three-body force, based on the
Maximum mass of neutron stars
We determine the structure of neutron stars within a Brueckner-Hartree-Fock approach based on realistic nucleon-nucleon, nucleon-hyperon, and hyperon-hyperon interactions. Our results indicate rather
Microscopic three-body forces and kaon condensation in cold neutrino-trapped matter
We investigate the composition and the equation of state of the kaon condensed phase in neutrino-free and neutrino-trapped star matter within the framework of the Brueckner-Hartree-Fock approach with
Asymmetric nuclear matter equation of state.
TLDR
The present calculations of the incompressibility predict a strong softening of the equation of state going from symmetric to asymmetric nuclear matter.
Equation of state of nucleon matter and neutron star structure
Properties of dense nucleon matter and the structure of neutron stars are studied using variational chain summation methods and the new Argonne ${v}_{18}$ two-nucleon interaction, which provides an
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