The paper by Paweł Danielewicz, Roy Lacey, and William G. Lynch discusses the determination of the equation of state (EOS) of dense matter through the analysis of nuclear collisions. These collisions can compress nuclear matter to densities similar to those found in neutron stars and core-collapse supernovae. The authors extracted pressures exceeding \(10^{34}\) pascals, the highest recorded under laboratory conditions. Using these data, they ruled out strongly repulsive EOSs from relativistic mean field theory and weakly repulsive EOSs with phase transitions at densities less than three times that of stable nuclei. However, they found that EOSs softened at higher densities due to a transformation to quark matter were not excluded. The nucleon-nucleon interaction is generally attractive at separations of 1 to 2 fm but becomes repulsive at smaller distances, making nuclear matter difficult to compress. Most stable nuclei have a saturation density of approximately \(2.7 \times 10^{14}\) g/cm\(^3\). The EOS of dense matter governs the compression in supernovae and neutron stars, as well as their internal structure and other properties. Nuclear collisions provide a means to compress nuclear matter to high density in a laboratory environment. The pressures resulting from these collisions influence the motion of ejected matter and provide sensitivity to the EOS. The authors applied a model within relativistic Landau theory to relate experimental observables to the EOS and other microscopic sources of pressure. They analyzed the flow of particles from the high-density region, which is sensitive to the EOS. The pressure can be calculated from the energy density and the baryon density using Boltzmann equations. The authors compared experimental data on transverse and elliptic flow to theoretical predictions, finding that no single EOS fully reproduced all the data. However, they constrained the EOS for symmetric nuclear matter, ruling out very repulsive EOSs and very soft EOSs with a strong phase transition at densities below three times the saturation density. They also discussed the implications of these constraints for the properties of neutron stars and supernovae.The paper by Paweł Danielewicz, Roy Lacey, and William G. Lynch discusses the determination of the equation of state (EOS) of dense matter through the analysis of nuclear collisions. These collisions can compress nuclear matter to densities similar to those found in neutron stars and core-collapse supernovae. The authors extracted pressures exceeding \(10^{34}\) pascals, the highest recorded under laboratory conditions. Using these data, they ruled out strongly repulsive EOSs from relativistic mean field theory and weakly repulsive EOSs with phase transitions at densities less than three times that of stable nuclei. However, they found that EOSs softened at higher densities due to a transformation to quark matter were not excluded. The nucleon-nucleon interaction is generally attractive at separations of 1 to 2 fm but becomes repulsive at smaller distances, making nuclear matter difficult to compress. Most stable nuclei have a saturation density of approximately \(2.7 \times 10^{14}\) g/cm\(^3\). The EOS of dense matter governs the compression in supernovae and neutron stars, as well as their internal structure and other properties. Nuclear collisions provide a means to compress nuclear matter to high density in a laboratory environment. The pressures resulting from these collisions influence the motion of ejected matter and provide sensitivity to the EOS. The authors applied a model within relativistic Landau theory to relate experimental observables to the EOS and other microscopic sources of pressure. They analyzed the flow of particles from the high-density region, which is sensitive to the EOS. The pressure can be calculated from the energy density and the baryon density using Boltzmann equations. The authors compared experimental data on transverse and elliptic flow to theoretical predictions, finding that no single EOS fully reproduced all the data. However, they constrained the EOS for symmetric nuclear matter, ruling out very repulsive EOSs and very soft EOSs with a strong phase transition at densities below three times the saturation density. They also discussed the implications of these constraints for the properties of neutron stars and supernovae.