ar X iv : h ep - p h / 05 11 09 2 v 2 1 6 N ov 2 00 5 Energy and system size dependence of chemical freeze - out in relativistic nuclear collisions

ar X iv : h ep - p h / 00 03 26 4 v 1 2 7 M ar 2 00 0 Time Dependence of Chemical Freeze - out in Relativistic Heavy Ion Collisions

ar X iv : h ep - p h / 06 07 16 4 v 1 1 4 Ju l 2 00 6 Status of Chemical Freeze - Out

The status of the energy dependence of the chemical freeze-out temperature and chemical potential obtained in heavy ion collisions is presented. Recent proposals for chemical freeze-out conditions are compared.

ar X iv : h ep - p h / 03 11 02 0 v 1 3 N ov 2 00 3 System - Size Dependence of Strangeness Saturation

The final state in heavy-ion collisions has a higher degree of strangeness saturation than the one produced in collisions between elementary particles like p − p or p − ¯ p. A systematic analysis of this phenomenon is made for C − C, Si − Si and P b − P b collisions at the CERN SPS collider and for Au − Au collisions at RHIC and at AGS energies. Strangeness saturation is shown to increase smoot...

11 09 2 v 1 8 N ov 2 00 5 Energy and system size dependence of chemical freeze - out in relativistic nuclear collisions

We present a detailed study of chemical freeze-out in p-p, C-C, Si-Si and Pb-Pb collisions at beam momenta of 158A GeV as well as Pb-Pb collisions at beam momenta of 20A, 30A, 40A and 80A GeV. By analyzing hadronic multiplicities within the statistical hadronization model, we have studied the parameters of the source as a function of the number of the participating nucleons and the beam energy....

ar X iv : h ep - p h / 05 07 27 6 v 1 2 5 Ju l 2 00 5 System - size dependence of strangeness production in high - energy A +

We argue that the shape of the system-size dependence of strangeness production in nucleus-nucleus collisions can be understood in a picture that is based on the formation of clusters of overlapping strings. A string percolation model combined with a statistical description of the hadronization yields a quantitative agreement with the data at √ s N N = 17.3 GeV. The model is also applied to RHI...