Nuclear Equation of State: Picture from Medium Energy Heavy Ion Collisions
P. Danielewicz
Abstract
Characteristics of the nuclear equation of state (EOS) and its importance, in particular for astrophysics, are discussed. Selected observables in nuclear collisions are sensitive to the EOS and can be used to constrain it. For central collisions, these include collective flow asymmetries, subthreshold kaon yields and isospin diffusion. Comparisons between the data and transport theory suggest an energy per nucleon that rises relatively slowly with density for symmetric matter and symmetry energy that rises relatively quickly around the normal nuclear density.
Create a lesson
Related papers
Quantum information in neutron-proton scattering from the M matrix
Linjun Xie, Jinniu Hu, Ying Zhang et al.
Local-nuclear-density dependent calculation of nucleon electromagnetic form factor ratios in finite nuclei
G. Ramalho, K. Tsushima, Myung-Ki Cheoun
Strongly coupled quark matter in neutron stars and their mergers
Konstantin Maslov, Ralf Rapp, Joaquin Grefa et al.
Implications of relativistic corrections on high-momentum nucleon-transfer reactions
W. L. Hai, D. Y. Pang, I. Tanihata et al.
Spin-State Teleportation and Tests of EPR Correlations Using 151 MeV Entangled Protons
H. Witała
Hadronic rescattering effects on net-proton cumulants from functional renormalization group calculations
Qianru Lin, Shi Yin, Jianing Li et al.