Heavy ion collisions with A = 10^{57}: Aspects of nuclear stability and the nuclear equation of state in coalescing neutronstar 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 heavyelement nucleosynthesis. The input physics for the study of such systems is similar to that required for the study of heavyion 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 neutronstar systems. The properties of the massradius 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 rapidneutron capture (rprocess) nucleosynthesis.
 Publication:

Presented at the Symposium on Hot Nuclei
 Pub Date:
 December 1987
 Bibcode:
 1987honu.symp.....M
 Keywords:

 Heavy Ions;
 Neutron Stars;
 Nuclear Fusion;
 Particle Collisions;
 Astrophysics;
 Binary Stars;
 Coalescing;
 Equations Of State;
 Gravitational Waves;
 Hydrodynamics;
 Stability;
 Astrophysics