Heavy ion collisions with A = 1057: Aspects of nuclear stability and the nuclear equation of state in coalescing neutron-star binary systems
Abstract
The dynamics of the final stages of the coalescence of two neturon stars (such as the binary pulsar PSR 1913+16) is an unsolved problem in astrophysics. Such systems are probably efficient generators of gravitational radiation, and may be significant contributors to heavy-element nucleosynthesis. The input physics for the study of such systems is similar to that required for the study of heavy-ion collision hydrodynamics; e.g., a finite temperature nuclear equation of state, properties of nuclei away from stability, etc. We discuss the development of a relativistic hydrodynamics code in three spatial dimensions for the purpose of studying such neutron-star systems. The properties of the mass-radius relation (determined by the nuclear equation of state) may lead to a proposed mechanism by which hot, highly neutronized matter is ejected from the coalescing stars. This material is photodisintegrated into a free (mostly) neutron gas which may subsequently experience rapid-neutron capture (r-process) nucleosynthesis.
- Publication:
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Presented at the Symposium on Hot Nuclei
- Pub Date:
- December 1987
- Bibcode:
- 1987honu.symp.....M
- Keywords:
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- Heavy Ions;
- Neutron Stars;
- Nuclear Fusion;
- Particle Collisions;
- Astrophysics;
- Binary Stars;
- Coalescing;
- Equations Of State;
- Gravitational Waves;
- Hydrodynamics;
- Stability;
- Astrophysics