The deformed projectiles and targets are expected to play different roles in heavy-ion collisions (HICs) at intermediate energy compared with spherical ones. With an isospin dependent quantum molecular dynamics (IDQMD) model, in despite of averaging all the orientations of axisymmetric deformed 24 Mg + 24 Mg collisions, it is still found that NN collision number, nuclear stopping power (R) and multiplicity of fragments have considerable differences compared with spherical 24 Mg + 24 Mg collisions.
AbstractDynamical interactions that occur between objects in dense stellar systems are particularly important for the question of formation of X-ray binaries. We present results of numerical simulations of 70 globular clusters with different dynamical properties and a total stellar mass of 2×107M⊙. We find that in order to retain enough neutron stars to match observations we must assume that NSs can be formed via electron-capture supernovae. Our simulations explain the observed dependence of the number of LMXBs on “collision number” as well as the large scatter observed between different globular clusters. For millisecond pulsars, we obtain good agreement between our models and the numbers and characteristics of observed pulsars in the clusters Terzan 5 and 47 Tuc.
Publisher's Note: “Molecular dynamics simulation of rotational relaxation in nitrogen: Implications for rotational collision number models” [Phys. Fluids 24, 106101 (2012)]
