The Equation of State of Dense Matter : from Nuclear Collisions to Neutron Stars
arXiv:0707.4067 · doi:10.1088/0954-3899/35/1/014048
Abstract
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 (NJL) and the Color Dielectric (CD) models, and found that the NS maximum masses are not larger than 1.7 solar masses. A comparison with available data supports the idea that dense matter EoS should be soft at low density and quite stiff at high density.
arXiv comment8 pages, 5 figures, invited talk given at NPA3, Dresden, March 2007
References in corpus (18)
- An accurate nucleon-nucleon potential with charge-independence breaking
- The equation of state for nucleon matter and neutron star structure
- Determination of the Equation of State of Dense Matter
- Hyperon stars in the Brueckner-Bethe-Goldstone theory
- A 2.1 Solar Mass Pulsar Measured by Relativistic Orbital Decay
- Evidence for a Soft Nuclear Equation-of-State from Kaon Production in Heavy Ion Collisions
- Effective Nucleon Masses in Symmetric and Asymmetric Nuclear Matter
- Quantum Monte Carlo Calculations of Neutron Matter
- Neutron stars and the transition to color-superconducting quark matter
- The Relativistic Dirac-Brueckner Approach to Asymmetric Nuclear Matter
- Covariant representations of the relativistic Brueckner T-matrix and the nuclear matter problem
- The Puzzles of RX J1856.5-3754: Neutron Star or Quark Star?
- Hybrid stars with the color dielectric and the MIT bag models
- Dirac-Brueckner-Hartree-Fock calculations for isospin asymmetric nuclear matter based on improved approximation schemes
- Neutron star properties and the equation of state of neutron-rich matter
- Azimuthal dependence of collective expansion for symmetric heavy ion collisions
- Neutron Stars and Massive Quark Matter
- Microscopic three-body forces and kaon condensation in cold neutrino-trapped matter