CERN Heavy Ion Forum

Nuclear Equation of State

Name: Nuclear Equation of State
Start: 2001-12-18T14:00:00+01:00
End: 2001-12-18T15:00:00+01:00
Location: CERN

by Pawel Danielewicz (Michigan State University and GSI Darmstadt)

Tuesday 18 Dec 2001, 14:00 → 15:00 Europe/Zurich

40-SS-C01 (CERN)

40-SS-C01

CERN

Description

The importance and status of the nuclear equation of state is discussed. The evolution of the early Universe depends on the phase transition from quark-gluon plasma to hadronic matter. The supernova explosions, stability of neutron stars and neutron star collisions, all depend on the stiffness of the equation of state at supranormal baryon densities. Since the equation also impacts nuclear reactions, those can be used to assess the features of the equation. Analysis of giant resonances constraints the nuclear incompressibilty. Analysis of flow in central collisions of heavy nuclei, at beam energies per nucleon between 0.1 GeV and 11. GeV, constraints nuclear pressure at supranormal baryon densities, 2 < rho/rho_0 < 5. The directional features of the flow probe the pace of expansion of the compressed participant matter and thus the pressure.

Organiser(s): Yiota Foka, Guy Paic and Urs Wiedemann