Recent progress constraining the nuclear equation of state from astrophysics and heavy ion reactions

Abstract

The quest for the nuclear equation of state (EoS) at high densities and/or extreme isospin is one of the longstanding problems of nuclear physics. Ab initio calculations for the nuclear many-body problem make predictions for the density and isospin dependence of the EoS far away from the saturation point of nuclear matter. On the other hand, in recent years substantial progress has been mode to constrain the EoS both, from the astrophysical side and from accelerator based experiments. Heavy ion experiments support a soft EoS at moderate densities while recent neutron star observations require a ``stiff'' high density behavior. Both constraints are discussed and shown to be in agreement with the predictions from many-body theory.

Invited talk given at NPA III, Dresden, Germany, March 2007

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Cited by in corpus (15)

• Hypernuclear Physics for Neutron Stars
• Phase transitions in dense matter and the maximum mass of neutron stars
• On the Maximum Mass of Neutron Stars
• Existence of hyperons in the pulsar PSRJ1614-2230
• Constraints for weakly interacting light bosons from existence of massive neutron stars
• Nuclear matter at high density: Phase transitions, multiquark states, and supernova outbursts
• Dynamical phase transition in neutron stars
• Density dependence of symmetry free energy of hot nuclei
• Remarks on the origin of Castillejo-Dalitz-Dyson poles
• Probing the momentum dependence of medium modifications of the nucleon-nucleon elastic cross sections
• The influence of reconstruction criteria on the sensitive probes of the symmetry potential
• The high density equation of state: constraints from accelerators and astrophysics
• Warm alpha-nucleon matter
• Nuclear equation of state and finite nucleon volumes
• Neutron star versus heavy-ion data: is the nuclear equation of state hard or soft?