Determination of the Equation of State of Dense Matter
By P. Danielewicz, R. Lacey, W. G. Lynch. Science, 2002
1,069 citations recorded by the source corpus.
Nuclear collisions can compress nuclear matter to densities achieved within neutron stars and within core-collapse supernovae. These dense states of matter exist momentarily before expanding. We analyzed the flow of matter to extract pressures in excess of 1034 pascals, the highest recorded under laboratory-controlled conditions. Using these analyses, we rule out strongly repulsive nuclear equations of state from relativistic mean field theory and weakly repulsive equations of state with phase transitions at densities less than three times that of stable nuclei, but not equations of state softened at higher densities because of a transformation to quark matter.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/51bf953a36ae1c7fdf2089996731158fbeb2a35e
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Citations in the corpus
- Symmetry Parameter Constraints from a Lower Bound on Neutron-matter Energy (2016, background): “Cai & Chen (2014) have argued, based on heavy-ion flow data analyzed by Danielewicz et al. (2002) and the existence of 2Me neutron stars, that −494MeV<Q0<−10MeV.”
- Combined Constraints on the Equation of State of Dense Neutron-rich Matter from Terrestrial Nuclear Experiments and Observations of Neutron Stars (2018, methodology): “Danielewicz et al. (2002).”
- Analytical representations of unified equations of state of neutron-star matter (2004, methodology): “As demonstrated by Gale et al. (1990), the flow is generated during the early nonequilibrium stages of the collision, whereas the interpretation in terms of the EoS by Danielewicz et al. (2002) is an equilibrium version of a simplified momentum-dependent interaction.”
- The Nuclear Symmetry Energy (2016, methodology): “[98], which indicate that these EOS are characterized by a symmetry energy compatible with phenomenology and observational 31”