Determination of the Equation of State of Dense Matter

2002/08/31 by P. Danielewicz, R. Lacey, W. G. Lynch · 3 citations
Physics and Astronomy · #nucl-th

paper · pdf · doi:10.1126/science.1078070

published as Science 298 (2002) 1592-1596 · 26 pages, 6 figures; final version

arxiv created 2003/01/22 · arxiv updated 2009/12/01

Abstract

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.

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