7 research outputs found
Recommended from our members
Thermal and dynamic multifragmentation of hot nuclei similarities and differences
The experimental data on fragment multiplicities, their energy and charge distributions, the emission times are considered for the nuclear multifragmentation process induced by relativistic light projectiles (protons, helium) and heavy ions. With light projectiles, the multifragmentation is a pure "thermal" process, well described by the statistical models. Heavy-ion-induced multifragmentation is influenced by dynamic effects related first of all to the compression of the system in the collision. But statistical models can also be applied to rendering the partition of the system if the excitation energy is less than 10 MeV/nucleon and compression is modest. For the central collision of heavy ions the statistical approach fails to describe the data
Recommended from our members
Phase transitions in highly excited nuclei
Phase transition in highly excited nucleus is treated in terms of thermo-dynamics of microensembles. The emission of intermediate mass fragments from pure thermally excited heavy nucleus Au is an indication of the liquid to fog phase transition. Evidence of the spinodal decomposition of the heavy nuclear system is found and its relation to the multisaddle transition configuration and freeze-out state is presented. 19
Recommended from our members
Phase transitions in highly excited nuclei
Phase transition in highly excited nucleus is treated in terms of thermo-dynamics of microensembles. The emission of intermediate mass fragments from pure thermally excited heavy nucleus 197Au is an indication of the liquid to fog phase transition. Evidence of the spinodal decomposition of the heavy nuclear system is found and its relation to the multisaddle transition configuration and freeze-out state is presented
Nuclear Equation of state for Compact Stars and Supernovae
International audienceThe equation of state (EoS) of hot and dense matter is a fundamental input to describe static and dynamical properties of neutron stars, core-collapse supernovae and binary compact-star mergers. We review the current status of the EoS for compact objects, that have been studied with both ab-initio many-body approaches and phenomenological models. We limit ourselves to the description of EoSs with purely nucleonic degrees of freedom, disregarding the appearance of strange baryonic matter and/or quark matter. We compare the theoretical predictions with different data coming from both nuclear physics experiments and astrophysical observations. Combining the complementary information thus obtained greatly enriches our insights into the dense nuclear matter properties. Current challenges in the description of the EoS are also discussed, mainly focusing on the model dependence of the constraints extracted from either experimental or observational data (specifically, concerning the symmetry energy), the lack of a consistent and rigorous many-body treatment at zero and finite temperature of the matter encountered in compact stars (e.g. problem of cluster formation and extension of the EoS to very high temperatures), the role of nucleonic three-body forces, and the dependence of the direct URCA processes on the EoS